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NTIFIC AS
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EISCAT Radar Systems
Location

Tromsø

Geographic coordinates69◦ 35’N
19◦ 14’E77◦ 30’N
66◦ 12’N

Geomagnetic inclination
Invariant latitude
Band
Frequency (MHz)Maximum bandwidth (MHz)Transmitter
Channels
Peak Power (MW)Average power (MW)
Pulse duration (ms)Phase coding
Minimum interpulse (ms)Receiver
System temperature (K)Digital processing
Antenna
Feed system
Gain (dBi)
Polarisation

KirunaSodankylä67◦ 52’N
67◦ 22’N20◦ 26’E26◦ 38’E76◦ 48’N76◦ 43’N64◦ 27’N
63◦ 34’N
VHF
UHF
UHF
UHF
224
931
931
931
3
8
8
8
1 klystron2 klystrons
8
8
8
8
1.6
2.0
0.20
0.25
0.001–2.0
0.001–2.0
binarybinarybinarybinary1.0
1.0
analoganaloganaloganalog
250–300
90–11050
50
14 bit ADC, 32 bit complex, autocorrelation functions, parallel channels
parabolic cylinder
120 m×40 m steerable
line feed
128 crossed dipoles
46
circularparabolic dish32 m steerable
Cassegrain

parabolic dish32 m steerable
Cassegrain

parabolic dish32 m steerable
Cassegrain

48.1
circular

48.1
any

48.1
any

Longyearbyen78◦ 09’N
16◦ 01’E82◦ 06’N75◦ 18’NUHF500
1016 klystrons
6
1.0
0.25
0.0005–2.0
binary0.1
analog
65–80
12 bit ADC, lag profiles
32 bit complex
Antenna 1
Antenna 2
parabolic dishparabolic dish32 m steerable
42 m fixed
Cassegrain
Cassegrain
42.5
circular

44.8
circular

EISCAT Heating Facility in TromsøFrequency range: 4.0–8.0 MHz, Maximum transmitter power: 12×0.1 MW, Antennas: Array 1 (5.5–8.0 MHz)
30 dBi, Array 2 (4.0–5.5 MHz) 24 dBi, Array 3 (5.5–8.0 MHz) 24dBi.
Additionally, a Dynasonde is operated at the heating facility.

Cover picture: Solar activity dependence of ion upflow in the polar ionosphere,
from the article by Y. Ogawa et al. (2010).

CAT SSICE

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EISCAT Scientific Association
2010

EISCAT, the European Incoherent Scatter Scientific Association, is established to conduct research on
the lower, middle and upper atmosphere and the ionosphere using the incoherent scatter radar technique.
This technique is the most powerful ground-based tool for these research applications. EISCAT is also
being used as a coherent scatter radar for studying instabilities in the ionosphere, investigating thestructure and dynamics of the middle atmosphere, studying meteors and as a diagnostic instrument inionospheric modification experiments with the heating facility.
There are fourteen incoherent scatter radars in the world, and EISCAT operates three of the higheststandard facilities. The EISCAT sites are located north of the Arctic Circle in Scandinavia. They consistof two independent radar systems on the mainland, together with a radar constructed on the islandof Spitzbergen in the Svalbard archipelago — the EISCAT Svalbard Radar (see sketch and operating
parameters on the inside of the front cover).
The EISCAT UHF radar operates in the 931 MHz band with a peak transmitter power of 2.0 MW,
and employs fully steerable 32 m parabolic dish antennas. The transmitter for this system and one of
the receivers are located in Tromsø (Norway). Receiving sites are also located in Kiruna (Sweden) andSodankylä (Finland), allowing for tri-static radar measurements.
The monostatic VHF radar in Tromsø operates in the 224 MHz band with a peak transmitter power of
1.6 MW, using a 120 m × 40 m parabolic cylinder antenna which is subdivided into four sectors. Thisantenna can be steered mechanically in the meridional plane from vertical to 60◦ north of the zenith;
limited east-west steering is also possible using alternative phasing cables.
The EISCAT Svalbard radar (ESR), located near Longyearbyen, operates in the 500 MHz band witha peak transmitter power of 1.0 MW, and employs a fully steerable parabolic dish antenna of 32 m
diameter and a fixed antenna, aligned with the local magnetic field, with a 42 m diameter. The highlatitude location of this facility is particularly aimed at studies of the cusp and the polar cap region.
The basic data measured with the incoherent scatter radar technique are profiles of electron density,
electron and ion temperatures and bulk ion velocity. Subsequent processing allows derivation of a wealthof further parameters, describing the ionosphere and neutral atmosphere. A selection of well-designed
radar pulse schemes are available to adapt the data-taking routines to many particular phenomena,
occurring at altitudes from about 50 km to above 2000 km. Depending on geophysical conditions, abest time resolution of less than one second and an altitude resolution of a few hundred meters can beachieved.
Operations of 3000–4000 hours each year are distributed between Common Programmes (CP) andSpecial Programmes (SP). At present, six well-defined Common Programmes are run regularly, forbetween one and three days, typically about once per month, to provide a data base for long term synoptic
studies. A large number of Special Programmes, defined individually by Associate scientists, are run tosupport national and international studies of both local and global geophysical phenomena.
Further details of the EISCAT system and its operation can be found in various EISCAT reports, including illustrated brochures, which can be obtained from EISCAT Headquarters in Kiruna, Sweden.

The investments and operational costs of EISCAT are shared between:
China Research Institute of Radiowave Propagation, Peoples Republic of China
Deutsche Forschungsgemeinschaft, Germany
National Institute of Polar Research, Japan
Natural Environment Research Council, United Kingdom
Norges forskningsråd, Norway
Solar-Terrestrial Environment Laboratory, Nagoya University, Japan
Suomen Akatemia, Finland
Vetenskapsrådet, Sweden

4

Contents
The Council Chairperson’s section

7

EISCAT_3D

8

Scientific highlights 2010
Mesospheric studies . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Spectral widths of polar mesospheric summer echoes . . . . . . . . . . . . . . . . . . . . .
Study of layered dusty plasma structures in the summer polar mesopause . . . . . . . . .
Polar mesosphere winter echoes . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Thermospheric studies . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Tidal waves in the polar lower thermosphere . . . . . . . . . . . . . . . . . . . . . . . . . .
SCANDI, an all-sky Doppler imager for studies of thermospheric spatial structure . . . .
Lower-thermospheric wind fluctuations . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Ionospheric studies . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Solar activity dependence of ion upflow in the polar ionosphere . . . . . . . . . . . . . . .
EISCAT observation of quiet-time ionospheric trough . . . . . . . . . . . . . . . . . . . . .
Spectrally uniform scattering cross section enhancements and ion-acoustic solitary waves
Enhanced ion acoustic line in the high ionosphere . . . . . . . . . . . . . . . . . . . . . . .
Statistical investigation of the Cowling channel efficiency in the auroral zone . . . . . . .
Comparison of EISCAT and SuperDARN F-region measurements . . . . . . . . . . . . . .
Polar cap studies . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Multi-radar study of global polar cap patch dynamics and morphology . . . . . . . . . . .
Seasonal influence on polar cap patches in the high-latitude nightside ionosphere . . . . .
Observations of polar cap patches with the ESR and rockets . . . . . . . . . . . . . . . . .
The open-closed field line boundary . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Polar cap boundary location using IMAGE and EISCAT . . . . . . . . . . . . . . . . . . . .
Polar cap signatures . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Studies of particle precipitation and the aurora . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Determination of the characteristic energy of precipitating electrons . . . . . . . . . . . . .
Acceleration mechanism for flickering aurora . . . . . . . . . . . . . . . . . . . . . . . . . .
Studies of dust and meteorites . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
ECOMA sounding rocket campaign . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Solar wind studies . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Interplanetary scintillation observations . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Studies of fundamental plasma physics . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Ray tracing analysis of L mode pumping of the ionosphere . . . . . . . . . . . . . . . . . .
Observations of heating experiments in the low ionosphere in polar winter . . . . . . . .
Activities by the Arctic and Antarctic Research Institute (AARI) in 2010 . . . . . . . . . . .
UK studies involving artificial heating . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Inversion results of incoherent scatter spectra . . . . . . . . . . . . . . . . . . . . . . . . . .
Spectra of non-Maxwellian distributions . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
New radar techniques . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Simulation of post-ADC digital beamforming for large aperture array radars . . . . . . .

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List of publications 2010

37

EISCAT Operations 2010

40

List of meetings 201044

Staff celebrations 201045

Beynon medals

46

EISCAT organisational diagram 2010

47

Committee Membership and Senior Staff

48

Appendix: EISCAT Scientific Association Annual Report, 2010

51

The EISCAT Associates, December 2010

65

Contact Information

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6

The Council Chairperson’s section
In summer 2010 EISCAT started to graduallylose its unique capability of tri-static measurements as the frequency band used for the UHFradars was given to mobile phone operators in
Lapland. The demand from the science community still continued to be high for the all EISCAT facilities and therefore an important challenge for the Council was to make wise decisions
for ensuring continued operations with the aging
instrumentation.
The acceptance of EISCAT_3D to the ESFRI
roadmap was an important factor to open new opportunities for additional EU funding for the EISCAT_3D mission. The new Director of EISCAT, Dr.
Esa Turunen, together with Dr. Ian McCrea madethe valuable work to harvest these opportunities.
They collected a group of experienced EISCAT scientists who prepared a successful proposal to the
EU FP7 call dedicated to research infrastructure
preparatory phase activities. The EISCAT_3D Preparatory Phase (PP) started in autumn 2010. The
consortium conducting the PP work is led by EISCAT and it includes research institutes from thehost countries of the current EISCAT facilities andfrom the UK. Since the beginning of the project, its
progress reports have been one the most interesting items in the Council meetings’ Agenda.
It is obvious that EISCAT_3D-PP gives positive momentum also to the current EISCAT activities. Therefore, I hereby want to express Council’s warm acknowledgements to the EISCAT Executives and other partners in the PP consortiumfor their efforts in EISCAT_3D development. Having said this, however, I want to remind that although not all the current EISCAT member countries are involved directly in the PP-activities, the
EISCAT_3D mission will be a success only if thewhole Association joins the effort. The future EISCAT activities will get funding only if they aresupported by a multinational science community
which has the urge to make good science with the
combination of EISCAT_3D and ESR. In parallelwith the PP work, it will be important to pay attention also to the development of the ESR system.
Svalbard measurements will have a crucial role inmaintaining the scientific interest towards EISCAT
during the years when the mainland radars arerenovated. Therefore, the Council was glad to notice that the mission of China to extend the ESR
system with a third antenna started to take the firststeps from a proposal towards a concrete working
plan in 2010.
Economically difficult times in the Association
continued during 2009–2010 and the uncertain
conditions are likely to continue at least for somemore years. As a consequence from this situation
the working environment may not have been optimal in all respects for the EISCAT Staff. Despite of the challenging situation these people haveshown excellent performance both in conducting
the EISCAT standard operations and in EU project work. On behalf of the EISCAT Council I wantto thank the Staff members for taking care of the
primary business of the Association, i.e. maintaining the most versatile ISR system in the world. I’msure that the whole EISCAT research community
is ready to join in these acknowledgements. The
Director of EISCAT has done excellent work in advertising EISCAT_3D in several different forums.
He has also been a key person in the implementation of the new EISCAT peer-review program,where scientists from all countries, both inside andoutside EISCAT, can make proposals for new innovative EISCAT experiments. I have no difficulties to believe that his persistent and enthusiastic PR work will eventually attract some newuser groups for EISCAT and this way improve also
the economical situation of the Association.
The two year period as the Council Chairperson has been very rewarding time for me. Collaboration inside the Council, with the EISCAT Executives and with national funding agencies has
been fluent and a very teaching experience. Therefore, I wish to thank all those people with whom I
have been working in EISCAT business during the
Chairperson period.
Dr. Kirsti Kauristie
Chairperson, EISCAT Council

7

EISCAT_3D
On 30 April 2009, the four-year EISCAT_3D
Design Study was completed. It was supported by the Sixth Framework Programme of theEuropean Union. The goals of the Design Study
were to study the feasibility of constructing a third
generation incoherent scatter research radar, thatwould be using cutting-edge technology throughout, in order to provide an order-of-magnitude improvement in the temporal and spatial resolution
when replacing the existing aging EISCAT VHF
and UHF systems — and to produce a detailed
design for such a system. This was reported in the
EISCAT Annual Report 2009.
The next stage of the development of the EISCAT_3D project is the Preparatory Phase. In
the Preparatory Phase the aim is to ensure that
the EISCAT_3D project will reach a sufficientlevel of maturity with respect to technical, legal
and financial issues so that it will be possible
to begin construction of the EISCAT_3D radarsystem. Thanks to the inclusion of the EISCAT_3D project on the ESFRI Roadmap for Research Infrastructures in 2008, it was possible toapply for EU funding for the Preparatory Phasethrough EU Framework Programme 7, under thecall FP7-INFRASTRUCTURES-2010-1 (Construction of new infrastructures: providing catalytic
and leveraging support for the construction of
new research infrastructures). The funding application for the Preparatory Phase was submitted to the EU system in early December 2009. The
plan was for 48 months of work, and an amountof 6 Me was requested. Later, during the negotiations in June 2010, the budget was adjusted down to a requested amount of 4.5 Me fromthe European Commission in order for the EISCAT_3D Preparatory Phase project to be accepted. Thus, the work in the EISCAT_3D Preparatory Phase could start in October 2010.
The workplan for the EISCAT_3D Preparatory
Phase is divided into fourteen individual Work
Packages that are intended to cover the areas intended to be targeted by the Preparatory Phase.
The Work Packages are:
WP1 Project management and reporting
WP2 Legal and logistical issues
WP3 Science planning and user engagement
WP4 Outreach activities
WP5 Consortium building
WP6 Performance specification
WP7 Digital signal processing
WP8 Antenna, front end and time synchronisation
WP9 Transmitter development
WP10 Aperture synthesis imaging radar
WP11 Software theory and implementation
WP12 System control
WP13 Data handling and distribution
WP14 Mass production and reliability
The consortium involved in the EISCAT_3D
Preparatory Phase work includes eight partners.
These are EISCAT Scientific Association, University of Oulu (including Sodankylä GeophysicalObservatory), Luleå Technical University, Swedish
Institute of Space Physics, University of Tromsø,
STFC-RAL, National Instruments and the Swedish
Research Council (including Swedish National Infrastructure for Computing).
The EISCAT_3D Preparatory Phase started
formally on 1 October 2010, and the first EISCAT_3D General Assembly meeting was held on
8

Artist’s vision of the core EISCAT_3D antenna field.

and the specific EISCAT_3D Preparatory Phase actions. The 21 presentations at the meeting gave agood overview of the status within these themes.
The final three months of 2010 were also thefirst three months of the EISCAT_3D Preparatory
Phase. The focus during these months were to
start up get the project going. An example ofthe progress in the project during these months
are the establishment of the initial Science Working Group, a group that combines existing EISCAT
users with members of other science communities
so that during the lifetime of the EISCAT_3D Preparatory Phase it will be possible to cover all of the
EISCAT_3D related science themes. Another example of early progress in the project is the launchof the upgraded EISCAT_3D project web-site.
Outside of the EISCAT_3D Preparatory Phase,the second EISCAT_3D Users Meeting was held
19–21 May, 2010, at Ångström Laboratory in
Uppsala, Sweden, following the success of thefirst Users Meeting at the same location one year
earlier. This was an open meeting for the prospective users of the future EISCAT_3D facility. The
meeting was organised as a two-way communication exercise, where the plans for the EISCAT_3D
Preparatory Phase activities were presented to theuser community and the user community’s scientific requirements for the system were gathered.
In total 36 presentations on EISCAT_3D related
topics were presented, and it was decided tocontinue having EISCAT_3D Users Meetings in
Uppsala in May.
Dr. Anders Tjulin
Project Assistant, EISCAT Scientific Association

6 October 2010. The General Assembly is thedecision-making body of the EISCAT_3D Preparatory Phase consortium and it consists of one representative from each of the participating partners (two from the Coordinator, i.e. EISCAT).
The members of the General Assembly are Esa
Turunen (EISCAT), Henrik Andersson (EISCAT),
Cesar La Hoz (Univeristy of Tromsø), Jerker
Delsing (Luleå Technical University), Lars Eliasson (Swedish Institute of Space Physics), Anita Aikio (University of Oulu), Tomas Andersson(Swedish Research Council), Leif Johansson (National Instruments) and Richard Harrison (STFC).
One of the items at the first General Assembly
meeting was to decide the members of the EISCAT_3D Executive Board, which is the supervisory body for the execution of the EISCAT_3D Preparatory Phase. It was decided that the Executive Board would consist of Esa Turunen, Henrik
Andersson, Jonny Johansson (Luleå Technical University), Thomas Ulich (University of Oulu), and
Ian McCrea (STFC) with Anders Tjulin (EISCAT)
also attending the meetings. The Executive Board
has weekly tele-conferences, and also meet physically once every three months.
A kick-off meeting for the EISCAT_3D Preparatory Phase was held 21–22 October 2010 at
Clarion Hotel Stockholm. Representatives fromall Work Packages and all Project Partner institutes were present, as well as representatives fromthe European Commission and other people interested in the EISCAT_3D development. The threemain themes that was discussed during the meeting were public engagement, support activities

9

Scientific highlights 2010
Mesospheric studies
Spectral widths of polar mesosphericsummer echoes
A controversial discussion in the literature about
the agreement or disagreement of spectral widths(after conversion to Doppler-velocities) of Polar
Mesospheric Summer Echoes (PMSEs) observed
simultaneously with the EISCAT VHF and UHF
radars motivated a detailed investigation of this
topic. A much larger data set than in any ofthe previous studies has been analysed. The previous discussions only considered case studies
of a few minutes in length, whereas Strelnikova
and Rapp (2011) considered a total of 380 min(in total 760 samples) of simultaneous and common volume observations with these two radars.
In that study it is discussed whether PMSEs atthese two frequencies originate from the same coherent scattering mechanism or if different physical mechanisms are necessary to explain theseechoes. Both the shape and the width of theconsidered spectra were investigated and it was
found that (within the available spectral resolution) the VHF spectra are on average well described by a Gaussian shape (with spectral parameter n = 2), which is derived from a generalised formulation of the autocorrelation function,
whereas the UHF-spectra show a small deviationfrom this shape.
Figure 1 indicates that the spectral widths dolargely agree, but show a small systematic difference which can be explained by considering
the effect of beam-, shear-, and wave-broadening.
This means that the slightly different beam widthsof the VHF and UHF radars and the hence
slightly different illuminated volumes account forthe small systematic difference in mean spectral
width. Finally, it was demonstrated that the small
deviation of the UHF-spectra from a perfect Gaussian shape can be either due to relatively small
signal-to-noise ratios of the UHF-data and/or asuperposition of incoherent and coherent scatter incases where both contributions add equally to the10

Figure 1: Half width at half maximum measured
simultaneously with the UHF and VHF radars.
The red solid line shows a 1:1 slope. The blue dashdotted line shows the relationship of two spectral
widths as expected in the case of an incoherent
scatter mechanism.

total observed power. Since VHF PMSEs are muchstronger than the incoherent scatter background,
this effect cannot be recognized in VHF observations. This superposition effect may occasionallyalso lead to larger deviations between VHF and
UHF spectra and, hence, significantly narrower
UHF spectra. However, excluding these rather
rare and exotic cases, Strelnikova and Rapp (2011)concluded that the majority of the observations
are compatible with a single coherent scattering at
both VHF and UHF.
Vertical wind fluctuations have been investigated to discuss the contributions of atmosphericwave activity on the spectral width. Figure 2
demonstrates that these fluctuations are modulated periodically. From the power spectrum of themodulation a dominant period (∼13 min in thiscase) can be identified. The wave periods for EISCAT VHF radar estimates of vertical wind fluctuations are summarised in Fig. 3 where time peri-

Figure 2: Example of vertical wind measurement
and spectrum of wind fluctuations. This example
was taken on 13 July 2004 from 10:00 to 11:20 UT at
an altitude of 83.6 km.

Figure 4: Evolution of number density profiles due
to gravity wave modulation. The time interval
between each panel is 30 min (t = 0, 30, 60, 90,
120, 150 min), with the vertical wavelength of 3 km
for the gravity waves and an intrinsic period of
2 hours.

Study of layered dusty plasma structuresin the summer polar mesopause

Data from sounding rocket campaigns indicatethat the radar Signal to Noise Ratio (SNR), theelectron density and the dust charge density of thesummer polar mesosphere have obvious layered
structure.
Traditional hydrodynamic equations are adapted to build a one-dimensional theoretical model
to study the effect of gravity waves on the formation and evolution of layered dusty plasma structures near the polar summer mesospause region
that is associated with the Polar Mesosphere Summer Echoes (PMSEs). The proposed mechanism
puts emphasis on the charged ice particle motion
by gravity wave modulation, making a significant
contribution to the vertically transport of heavy ice
Figure 3: Histogram of wave periods derived fromthe spectral analysis of vertical wind observations
particle and convergence into thin layers. Figure 4
obtained from VHF PMSE data. The blue histoshows how a charged ice particle distribution withgram shows the results for all VHF PMSE observaan initial Gaussian shape transforms into distinct
tions in July 2004 and 2005 and the red histogramthin-layer structures.
shows the subset of data where UHF PMSE wereAs shown by Figs. 5 and 6, the pattern ofobserved simultaneously.
the multi-layer structure depends on the vertical
wavelength of the gravity waves and on the sizeof the ice particles. Based on the above mechods where PMSEs also occurred in the UHF radar anism, with the vertical wavelength 2.5 km andmeasurements are separated from periods where the period 4 hours, the experimental result recorthey did not. Both distributions show a maximum ded during the ECT02 sounding rocket campaign
of wave periods in the order of 5–10 min.
(Havnes et al., 1996) was reproduced as shown in
Figure 7.
In addition, based on the theory of wave
I. Strelnikova, and M. Rapp, “Majority of PMSE spectral propagation in layered media, SNR in polar mesowidths at UHF and VHF are compatible with a single sphere during PMSEs were studied. By comparing
scattering mechanism”, J. Atmos. Solar-Terr. Phys., the calculated and experimental results (Fig. 8),
the calculated SNR almost agrees with the experdoi:10.1016/j.jastp.2010.11.025, in press, 2011.
11

Figure 5:
The influence from the vertical
wavelength of the gravity waves on the formation of ice particle layers. The wavelengths are
λ = 3 km, 4 km and 5 km respectively.

Figure 8: Profile of the SNR measured with the
ALOMAR-SOUSY VHF radar during sounding
rocket flight ECT02 (solid line). Profiles of SNR calculated with the method of layered media (dashedline).

Figure 6: The effect on the formation of layer structures from different ice particle sizes. The sizes arerd = 10 nm, 30 nm and 50 nm respectively.

determined by fitting the auto-correlation functions using the algorithm discussed by Strelnikova
and Rapp (2010). Several models have been proFigure 7: Comparison between the ECT02 rocket
posed in the literature (e.g. turbulence or damped
sounding data (thin black line) and the model calviscosity waves) to explain these radar echoes occulations results (red line). The estimated verticalcurring at lower mesospheric altitudes than mesowavelength is 2.5 km and the period is 4 hours.
spheric summer echoes. Extracting the n parameters only for strong echoes show that inside theimental one, but there are still some differences strong PMWE the n parameters are similar to 2
between the calculated and the experimental res- which exhibits an Gaussian spectral shape. The
ults, which may be caused by the vacuum assump- analysis of the spectral shape supports the thetion at altitude 0–83 km and the neglected possible ory that turbulence is an important mechanism foreffects from the magnetic field. In fact, the mag- the occurrence of PMWEs. On the other hand,
netic field should not have any important impact the radar echoes observed with the EISCAT VHF
in the VHF and UHF bands, but when the obser- radar are too strong to be explained by turbulence
vation are carried out in the MF and HF bands the alone because extremely high turbulence activity
influence of magnetic field should be taken into ac- would have been necessary to achive such strong
echoes as those observed. Additional contribucount.
tions have to be considered to explain the physicalH. Li, et al., “Study on the layered dusty plasma struc- mechanism responsible for the occurrence of PMtures in the summer polar mesopause”, Ann. Geophys. WEs.
28, 1679–1686, 2010.

H. Li, et al., “Reflection characteristics of layered media
in polar mesopause occurring polar mesosphere summer echoes”, Plasma Science and Technology 12, 2010.

Polar mesosphere winter echoes
Polar Mesosphere Winter Echoes (PMWEs) havebeen analysed in great detail and the first results
have been presented (e.g. Engler et al., 2010a,b).
Figure 9 shows the statistics of the spectral shape
12

N. Engler, M. Rapp, and I. Strelnikova, “Analysis of thespectral form of polar mesosphere winter echoes measured with the eiscat-vhf-radar”, Talk at DPG Frühjahrstagung, Bonn, Germany, March 15–19, 2010a.
N. Engler, M. Rapp, and I. Strelnikova, “Analysis of polar mesosphere winter echoes using the EISCAT-VHFradar”, Poster at SCOSTEP-12 Symposium, Berlin, Germany, July 12–16, 2010b.
I. Strelnikova, and M. Rapp (2010), “Studies of polar mesosphere summer echoes with the EISCATevaluated, and it was shown that they were notcausing this. From the analysis of 22.5 days ofwind data, about 5–6 day oscillations were foundin the lower thermosphere, probably where there
were planetary wave activity in the lower thermosphere.
S. Nozawa, et al., “Tidal waves in the polar lower thermosphere observed using the EISCAT long run data set
obtained in September 2005”, J. Geophys. Res. 115,
A08312, doi:10.1029/2009JA015237, 2010.

Figure 9: Statistical analysis of the spectral form of
PMWEs. The majority of the observations show a
Lorentzian shape while inside strong PMWEs theGaussian shape dominates.
VHF and UHF radars: Information contained in the
spectral shape”, Adv.
Space Res.
45, 247–259,
doi:10.1016/j.asr.2009.09.007.

SCANDI, an all-sky Doppler imager forstudies of thermospheric spatial structure

Thermospheric studies

Aruliah et al. (2010) has presented the initial results from a new all-sky Fabry-Perot InterferoTidal waves in the polar lower thermo- meter (FPI) called the Scanning Doppler Imager
sphere(SCANDI), which has been built and installed atLongyearbyen, Svalbard, and was first operated
Characteristics of the lower thermospheric windin December 2006. SCANDI observes the Doppler
have been determined from a long run data set
shifts and Doppler broadening of the 630 nm airobtained by the EISCAT UHF radar at Tromsø
glow and aurora from which upper thermospheric◦◦(69.6 N, 19.2 E) over ∼23 days, from September 6
winds and temperatures can be calculated. The
to 29, 2005 (Fig. 10). The derived semidiurnal
imager allows measurements over a field-of-view
amplitude exhibited day-to-day variations (∼5–
(FOV) with a horizontal radius of nearly 600 km
30 m/s) at and above 109 km, while the phase varfor observations at an altitude of 250 km, using a
ied little with the day. A mode change was foundtime resolution of 8 minutes. SCANDI providesof the semidiurnal tide occurring during Septemthe ability to observe thermospheric spatial strucber 17–22, 2005. Between September 6 and 16 theture within a FOV which overlaps the FOVs of thevertical wavelengths were estimated to be ∼58 km
EISCAT Svalbard radar and CUTLASS SuperDand ∼76 km for the meridional and zonal componARN radars. Coordination with these instruments
ents, respectively, while between September 23
provides an important opportunity for studying
and 29 they became less than ∼24 km. Wind dataion-neutral coupling. The all-sky image is divided
from MF radars co-located at Tromsø, and also
into several sectors to provide a horisontal spatial
at Poker Flat, were also anaylsed. Comparison
resolution of between 100 and 300 km. The newof the wind data from the two MF radars indicinstrument represents a powerful extension in obated that migrating semidiurnal tide was dominservational capability but it requires careful calibating in the mesosphere. Furthermore, the verticalration and data analysis. Two observation modes
wavelengths (i.e., modes) were different to eachhave been used: one fixed and one scanning etother in the mesosphere and the lower thermoalon gap. SCANDI results have been corroborated
sphere for each interval. The day-to-day variabusing the Longyearbyen single look direction FPI,
ility of the diurnal tide was less obvious than thattogether with ESR measurements of the ion temof the semidiurnal tide. The diurnal amplitude ofperatures. The data reveal thermospheric temperthe meridional component increased with height
ature gradients of a few K/km and a great deal of
except for 8 days between September 13 and 20,
meso-scale variability, on spatial scales of several
when the diurnal amplitudes had smaller values
tens of kilometres.
(< 40 m/s) at and above 111 km than for the otherintervals. Furthermore, the shapes of the altitude
profiles of the meridional phase differ from those A. L. Aruliah, et al., “SCANDI an all-sky Doppler imfor the other intervals. Contributions due to the ager for studies of thermospheric spatial structure”,
electric field and the ion drag acceleration were Ann. Geophys. 28, 549–567, 2010.
13

Figure 11: Comparison of ion temperatures observed by the two ESR radars with the neutral temperatures observed by SCANDI on the night of 6–
7 February 2007.

Lower-thermospheric wind fluctuations

thermospheric wind velocity measured with the
FPI showed obvious fluctuations in both the vertical and the horisontal components. Of particularinterest is that the location of the fluctuations arefound in a darker area that appeared within thepulsating aurora. During the same time period the
EISCAT radar observed sporadic enhancementsin the F-region backscatter echo power, suggesting presence of low-energy electron (1 keV orlower) precipitation coinciding with an increasein the amplitude of the electromagnetic wave (atthe order of 10 Hz or higher). While the dominant mechanism causing the fluctuations in FPIderived wind velocity during the pulsating aurora
have not yet been identified, the frictional heating energy dissipated by the electric-field perturbations may be responsible for the increase in ionospheric thermal energy and thus modifying the
local wind dynamics in the lower thermosphere.

Simultaneous observations were conducted with a
Fabry-Perot Interferometer (FPI) at a wavelengthof 557.7 nm, an all-sky camera at a wavelengthof 557.7 nm, and the European Incoherent Scatter (EISCAT) UHF radar during the Dynamics
and Energetics of the Lower Thermosphere in
Aurora 2 (DELTA-2) campaign in January 2009
(Fig. 12). This study concentrates on two events
during periods of pulsating aurora. The lower-

S. Oyama, et al., “Lower-thermospheric wind fluctuations measured with an FPI in pulsating aurora atTromsoe, Norway”, Ann. Geophys. 28, 1847–1857,
2010.

Figure 10: Altitude profiles between 70 and 120 kmof the amplitudes (top panels) and the corresponding phases, i.e. the local time of maximum, (bottom
panels) of the semidiurnal tides for the meridional(left panels) and the zonal (right panels) components. Circles (and dashed lines) denote results fromthe 10 day data window starting at 19:00 UT on
September 6, while triangles (and solid lines) denote results from the 6 day data window startingat 07:00 UT on September 23. Larger filled symbols
denote data above 99% significance level, smaller
filled symbols denote data between 50% and 99%
significance levels, and open symbols denote data
below 50% significance level. EISCAT UHF data
are shown for altitudes at and above 96 km, while
Tromsø MF radar data are shown for altitudes atand below 91 km.

14activity than at low activity. Ion upflow events,
and also the upward velocity, behave the opposite: they are more frequent and at higher altitudes
at times of low solar activity. In any year about
30%–40% ion upflow is accompanied by ∼500 K
higher electron temperature than the backgroundtemperature at 400 km altitude. Electron and ion
heating in connection with upflow is nearly twiceas prevalent during high solar activity than at low
activity. The acceleration of ions by pressure gradients and ambipolar electric field becomes larger at
low solar activity compared to high activity. Thisvariation of the average acceleration is caused by
the different shape of the electron density profile
when the solar activity is low compared when it ishigh. Ions start to flow upward at above 450 km
altitude at high solar activity, and lower (at 300–
500 km altitude) at low solar activity. It is suggested that the solar activity influences the long-term
variations of the ion upflow occurrence because
it modulates the density of the neutral particles,
the formation of the F2 density peak, and the ionneutral collision frequencies in the thermosphereand ionosphere.

Figure 12: The top and middle panels show the
temporal variations in the vertical wind speed andthe fringe peak count at the zenith, respectively,
measured with the FPI (557.7 nm) from 00:30 to
02:00 UT on 26 January 2009. The vertical bars denote the 2σ uncertainty. The bottom panels show
horisontal aurora images taken with the ASC at
557.7 nm from 01:15 to 01:39 UT during pulsating
aurora (the corresponding time interval is marked
by black dashed line in the top two panels). The
colour scale of the optical intensity is shown at
centre right. These images are mapped in geographic coordinates assuming that the peak emission height is 110 km. The five black dots andthe four red crosses indicate the location of the
FPI and the EISCAT UHF radar observation positions, respectively. The black arrows correspondto the horizontal component of the FPI-derived
neutral wind velocity (the scale is presented at theright bottom corner of the first panel from the left).
White dashed lines are drawn in the colour panels
to easily identify the darker area.

Y. Ogawa, et al., “Solar activity dependence of ion upflow in the polar ionosphere observed with the EISCAT
Tromsø UHF radar”, J. Geophys. Res. 115, A07310,
doi:10.1029/2009JA014766, 2010.

EISCAT observation of quiet-time ionospheric troughIonospheric studies
Solar activity dependence of ion upflow
in the polar ionosphere
The influence of solar activity on ion upflow in thepolar ionosphere has been investigated using dataobtained by the European Incoherent Scatter (EISCAT) Tromsø UHF radar between 1984 and 2008.
In agreement with other work the upward ion flux
was generally found to be higher at high solar

Data from combined azimuth-scan and overheadscan UHF experiments were used to determine thebehaviour of the eveningside F-region trough on
9 November 1987. The MLT and CGMlat dependence of various ionospheric parameters at a set of
F region altitudes was determined. It was foundthat both ion and electron temperatures have minima within the trough region, and increase at thepoleward edge. The most important result was
obtained by comparing the observed ion velocity
and electron density to the respective parameters
given by the LiMIE model (see Fig. 14). The results suggest that the density depletion within thetrough is due to recombination of F-region plasma
convecting for a long time in the dusk convection
cell beyond the terminator. The northern edge ofthe trough is associated with soft particle precipitation. The southern edge is steeper than the northern one, and is built by sun-lit plasma brought tothe trough region by co-rotation. The trough isthus a result of a combination of transport and precipitation processes rather than stagnation.

15

Figure 13: (a) Occurrence frequency of ion upflow
starting between 200 and 550 km altitude in thenighttime between 19:00 and 05:00 MLT is shown
between 1984 and 2008: 1 year average (black line)
and 3 month average (gray circles). (b) Average
field-aligned ion velocity at 400 km altitude versus
year. Red circles indicate the average flux in upflow events, and blue circles indicate the average
flux of all samples (upflow, no-flow, and downflow
events). (c) Average field-aligned flux at 400 km
altitude versus year. These circles are plotted every
3 months.

Figure 15: Incoherent radar spectra obtained with
ESR. The left panel shows a typical NEIAL at altitudes above 300 km on 9 April 2007 at 11:31:54 UT.
The right panel shows a different kind of spectral
enhancement seen on 1 August 2007 at 00:43:00 UT.
Both spectra had 6 s integration time. The colour
bar shows the range corrected power spectral density in arbitrary units.

ent signal off ion-acoustic waves and Langmuir
waves in the ionosphere. Occasionally, the upshifted and/or downshifted lines produced by
the ion-acoustic waves are enhanced well above
thermal levels and referred to as Naturally Enhanced Ion-Acoustic Lines (NEIALs; Fig. 15, left
panel). At other times a different kind of enhancement is seen, which is spectrally uniform
over the whole ion-line, i.e. the up- and downshifFigure 14: Zonal ion velocity (left panel) and elected shoulder and the spectral valley in between
tron density (right panel) at 345 km together with
(Fig. 15 (right panel). Based on observations madethe convection pattern given by the LiMIE model.
with the EISCAT Svalbard Radar (ESR) facility,
Positive potential is indicated by continuous lines
the transient and spectrally uniform power enand negative potential by dashed lines. The posihancements were investigated and found to be extion of the solar terminator is also indicated in theplained by ion-acoustic solitary waves. A theory
plots as a line of contrasting colour.
of nonlinear waves in a magnetised plasma enables the determination of the properties of such
M. Voiculescu, et al., “An olden but golden EISCAT ob- waves and the evaluation of their effects on teh
servation of a quiet-time ionospheric trough”, J. Geo- scattered signals measured by the ESR. This newphys. Res. 115, A10315, doi:10.1029/2010JA015557, mechanism can explain backscattered power enhancements by one order of magnitude above the2010.
thermal level and is consistent with observations.

Spectrally uniform scattering cross section enhancements and ion-acoustic solitary waves
Spectra measured by incoherent scatter radars areformed predominantly by scattering of the incid16

J. Ekeberg, et al., “Ion-acoustic solitary waves and spectrally uniform scattering cross section enhancements”,
Ann. Geophys. 28, 1299–1306, doi:10.5194/angeo-281299-2010, 2010.

Figure 16: Ion acoustic spectra with different
electron-ion temperature ratio and different relative drift of the H+ and O+ ions.

Figure 17: Effects on the ion acoustic spectrum of
the relative amounts of H+ and O+ ions in theplasma.

Enhanced ion acoustic line in the highionosphere
The received power of scattered radar signals issometimes extremely enhanced to up to 2 times
above its usual values, and it is mostly containedin the two ion acoustic lines, often asymmetrically. The explanation to this phenomenon has inmany publications been proposed to be instability processes. One of these theories includes theion-ion two-stream instability, which is driven bylarge relative drifts between two or more ion species, for example a plasma with O+ with a beamof H+ . As long as the drift velocity is of the sameorder of magnitude as the species thermal velocity, the ion acoustic fluctuation level can be enhanced well above the thermal level leading to an
enhancement in one or both ion lines. The high relative drift velocity require sufficient accelerationof H+ which might be possible at high altitudes.

X. Kun, et al., “Interpretation on the origin of enhanced
ion acoustic line spectra in the high ionosphere”, Chin.
J. Space Sci. 30, 29–34, (in Chinese) 2010.

Statistical investigation of the Cowlingchannel efficiency in the auroral zone

The Cowling channel mechanism describes thecreation of a secondary polarisation electric field at
sharp conductance boundaries in the ionosphere
due to excess charges, in the case that the release of
these charges to the magnetosphere is fully or partially impeded. The secondary currents generated
by the polarisation electric field effectively modify
the effective ionospheric conductivity inside the
Cowling channel. While the Cowling mechanism
is generally accepted for the equatorial electrojet,
there is a long-standing discussion about the importance of this mechanism and its efficiency inthe auroral electrojet.
A statistical investigation is presented that en+Assuming low energy H ion precipitation andables
identification of the most probable geospace++
the O ion outflow events, and a H ion distribuconditions
and MLT locations for a high Cowltion function described by a bi-Maxwellian coning
efficiency.
This investigation is based on moretaining the field-aligned heat flow, the enhanced
than
1600
meridional
profiles of data from theion acoustic echoes can be interpreted using the
MIRACLE
networkinScandinavia, in particular
ion-ion two-stream instabilities. Then the asymgroundmagnetic
field
datafrom the IMAGE magmetry is weakened due to the consideration of
netometer
network
andelectric
field data fromfield-aligned heat flow.
the STARE radar, supported with pointwise ionoAs shown by Fig. 16, the asymmetry is weaker spheric conductance measurements from the EISwith increasing electron-ion temperature ratio CAT radar. The single point conductance measTe /Ti . Given a constant electron-ion temperature urement that EISCAT provides is crucially importratio, however, the incoherent scattering spectrum ant in order to overcome uncertainties caused by
grows gradually asymmetric when the two-ion re- unknown boundary values when solving for thelative drift velocity increase.
electrodynamic parameters along each meridional
The change in asymmetry and amplitude of profile. The data were analysed in the framework
the ion acoustic spectrum with different relative of a 3D ionospheric model, but the data set wasamount of H+ and O+ ions is shown in Fig. 17. Al- filtered such that only electrojet-type situations
though the amplitude of the ion acoustic spectrum were included, for which the gradients of all measis weaker with increasing H+ content, the corres- ured quantities in longitudinal direction could be
ponding non-asymmetry ratio of the ion acoustic neglected. The analysis results in a steep peak
spectrum grows more asymmetric.
of high Cowling channel efficiency probability in
17

Figure 19: SuperDARN and EISCAT velocity comparison for EISCAT CP-1 and CP-2 modes from1995 to 1999. SuperDARN points that showedeither high standard deviation or little data in thesurrounding cells were discarded.

Figure 18: The probability of high Cowling channel efficiency increases almost monotonically withincreasing geomagnetic activity.

the early morning sector (0245–0645 MLT), withthe largest probability around 05 MLT and for medium and high geomagnetic activity. In agreementwith an earlier single event study by Amm andFujii (2008), this indicates that the Cowling mechanism may be most effective in the early morningpart of the central substorm bulge. Further, thisanalysis results in an almost monotonic increase of
the probability of high Cowling channel efficiency
with increasing geomagnetic activity (see Fig. 18).

lower. Other estimates of ns were made using
electron densities based on both EISCAT measurements and values from the International Reference Ionosphere model, but these still did not increase the SuperDARN velocities enough to attainthe EISCAT values. Gillies et al. (2010) proposedthat small-scale dense structures with refractive
O. Amm, et al., “A statistical investigation of the Cowl- indices well below unity must exist within the Suing channel efficiency in the auroral zone”, J. Geophys. perDARN scattering volume and may contributeRes. 116, A02304, doi:10.1029/2010JA015988, 2011.
greatly to the scattering process. These dense, localised structures would provide the density gradiComparison of EISCAT and SuperD- ents required to generate the coherent irregularities from which the SuperDARN radar waves scatARN F-region measurements
ter, whereas EISCAT incoherent radar measureGillies et al. (2010) has compared line-of-sight ve- ments provide only the background Ne and notlocity measurements by SuperDARN with EIS- the density of the small-scale structures.
CAT tri-static velocity measurements made during
the period from 1995 to 1999. It was found thatthat the velocities measured by SuperDARN were
statistically lower than those measured by EISCAT. Part of the discrepancy could be attributed to
the fact that the SuperDARN analysis neglects thelower-than-unity refractive index of the scattering R. G. Gillies, et al., “A comparison of EISCAT and Sustructures. The elevation angle measured by Su- perDARN F-region measurements with consideration
perDARN was used as a proxy estimate of ns and of the refractive index in the scattering volume”, J. Geothis improved the comparison, but the velocities phys. Res. 115, A06319, doi:10.1029/2009JA014694,
measured by SuperDARN were still consistently 2010.
18

Figure 20: Observation of three polar cap patches
as they drift through the most vertical beam of the
Resolute Bay AMISR (RISR).

Figure 21: Polar cap patch one and two drifting
through the EISCAT Svalbard Radar 42 m beam.

Polar cap studies
Multi-radar study of global polar cap
patch dynamics and morphology
In December 2009 a multi radar/optical campaign
was performed in order to study the large scale
motion of polar cap patches across the polar cap.
This was a combined effort by scientists at the University of Tromsø, Boston University, SRI International and the US Air-force Research Laboratory.
Five high latitude incoherent scatter radars
were in operation simultaneously (PFISR, RISR,
Søndrestrøm, EISCAT UHF and EISCAT Svalbard
radar) as well as several all-sky imagers and ionosondes. The geomagnetic conditions during the
campaign were quiet and the auroral oval was attimes observed to be very small. Polar cap patches
were observed on a routine basis throughout the
campaign.
In Fig. 20 a series of three patches are observed
as they drift through the most vertical beam of
the Resolute Bay AMISR (RISR). All three patches
could be tracked optically with the all-sky imager
located in Qaanaaq as they drifted towards theEuropean sector. Figure 21 shows patch one andtwo as they drift through the ESR 42 m beam.
Patch three missed ESR due to the Earth’s rotationand entered the European sector west of Svalbard.
Figure 22 shows the trajectory of patch number
one as calculated by the Weimer statistical convection model. It clearly shows how the principal motion across the polar cap of large scale features likepolar cap patches can be successfully modelled using statistical models.

Figure 22: Trajectory of polar cap patch number
one calculated by the Weimer statistical convection
model.

Seasonal influence on polar cap patches
in the high-latitude nightside ionosphere

Three years of ESR data (1999–2001) were used by
Wood et al. (2010) to study the influence of seasonality on the patch-to-background density ratio ofpolar cap patches in the nightside ionosphere observed above northern Scandinavia around solar
maximum. Data were selected from periods favourable for patch formation, based on the highlatitude plasma convection pattern, the interplanetary magnetic field, and an absence of in situ
precipitation. Patch-to-background ratios of up
to 9.4 ± 2.9 were observed between midwinterand equinox, with values of up to 1.9 ± 0.2 insummer. As the patch-to-background ratios insummer were <2, the enhancements could notformally be called patches; however, they werestill significant density enhancements within theanti-sunward cross-polar flow. Aberystwyth University’s PLASLIFE (PLASma LIFEtime) computer
simulation was used to model the seasonal trend
in the patch-to-background ratio and to estabM. G. Johnsen, et al., “A multi radar study of global po- lish the reasons for the difference between winterlar cap patch dynamics and morphology”, to be submit- and summer values. This difference was primarted, summer 2011.
ily attributed to variations in the chemical com19

Figure 23: Patch-to-background ratios as a function of the number of days from winter solsticefor observations made between 1999 and 2001.
When the patch-to-background ratio is <2, theseenhancements are not formally defined as polar
cap patches.

position of the atmosphere, which, in summer,
both reduced the electron density of the plasma
drawn into the polar cap on the dayside and enhanced plasma loss by recombination. A secondary factor was the maintenance of the backgroundpolar ionosphere by photo-ionization in summer.
A. G. Wood and S. E. Pryse, “Seasonal influence on polar cap patches in the high-latitudenightside ionosphere”, J. Geophys. Res.
115,
A07311, doi:10.1029/2009JA014985, 2010.

Observations of polar cap patches with
the ESR and rockets
There have in recent years been several sounding
rocket campaigns at Svalbard. Burchill et al. (2010)
used ESR data to study the upflow of thermal ionsin the cusp region during the CUSP-2002 sounding rocket flight from Ny-Ålesund on 14 December 2002. They studied the correlation between ion
upflow, electron energy fluxes, convection electric fields, VLF/BBELF wave power, and parallel/perpendicular ion temperatures. Lorentzen etal. (2010) used ESR and ground-based optical data
to study the formation of a polar cap patch event
during the ICI-2 sounding rocket flight from NyÅlesund on 5 December 2008, and they developed
a conceptual model for how the polar cap patch
was created.
Oksavik et al. (2010) used ESR and SuperDARN data to study how two intense polar cap
patch events on 6 February 2001 drifted across thepolar cap from Svalbard to Alaska. Both events
had extremely high electron densities (exceeding
1012 m−3 ) when they were first discovered by the
ESR in the dayside cusp region over Svalbard, see
20

Fig. 24. On their way across the polar cap they
underwent pulsed flow and substantial rotation.
On the nightside the leading edge had become thetrailing edge. It suggests that the first patch toenter the dayside polar cap may not always be thefirst patch to reach the nightside. It also suggeststhat momentum transfer in the dayside polar cap
can last significantly longer than 10 minutes afterreconnection, especially for extremely long fieldlines when IMF By is dominating. Knowledge ofthe solar wind driver and the coupling processes
is therefore extremely important for predicting the
motion of polar cap patch events across the polar
cap. The gradients in the plasma flow associatedwith the rotation of the extreme density may initself lead to a stronger growth of ionospheric irregularities that may continue to grow all the way
across the polar cap. The result will be more efficient creation of ionospheric irregularities.
J. K. Burchill, et al., “Thermal ion upflow in thecusp ionosphere and its dependence on soft electron energy flux”, J. Geophys. Res. 115, A05206,
doi:10.1029/2009JA015006, 2010.
D. A. Lorentzen, et al., “In situ measurements of a newly
created polar cap patch”, J. Geophys. Res. 115, A12323,
doi:10.1029/2010JA015710, 2010.
K. Oksavik, et al., “On the entry and transit of highdensity plasma across the polar cap”, J. Geophys. Res.
115, A12308, doi:10.1029/2010JA015817, 2010.

The open-closed field line boundary
In s study by Woodfield et al. (2010) previous work
was revisited which used two EISCAT radars to
track the motion of the Open-Closed field line
Boundary (OCB). The location of the OCB enables
the size of the polar cap to be established, which isvery important for understanding substorm processes and reconnection rates in general. In previous studies, one radar was used to observe thelatitudinal variation of F-region electron temperature, while the second one was used to estimate thebackground variation of Te with altitude which
was then subtracted from the measurements inthe first radar beam in order to identify the electron temperature enhancement corresponding to
the OCB. Woodfield et al. demonstrated that theuse of a model such as the International Reference Ionosphere 2007 (IRI-2007) can remove therequirement for the second radar and therefore
increase the number of cases in which the background Te subtraction can be performed. Applying the modified technique to some substormFigure 25: The data are from 29 October 2004. (aand c) ∆Te with overlaid bTe (black line) from the
IRI (Tet =100 K) and ESR (Tet =500 K) methods,
respectively; (b and d) the full range of boundaries from Tet ranging from -500 to 500 K for the
IRI and ESR methods, respectively; (e) bTe fromthe IRI and ESR methods (vertical white on blackline is substorm onset time from the Frey et al.
(2004) list, and yellow stars indicate DMSP b6 identifications); (f) Pi2 filtered (20–200 s) H component
magnetometer data from Lerwick, United Kingdom; (g) H component magnetometer data from
Kilpisjärvi, Finland.

Figure 24: ESR and SuperDARN data of two intense polar cap patch events on 6 February 2001
drifting across the polar cap from Svalbard to
Alaska.

observations of the EISCAT radar facility wereused to estimate the latitude of the PCB along themeridian of the EISCAT VHF beam. The second
method for estimating PCB utilised global imagesof proton aurora obtained by the FUV SI12 instrument of the IMAGE satellite. In two events, theagreement between the two methods was good
and the mean of the difference was within the resolution of the observations (see Fig. 26). In a third
event, the PCB estimated from EISCAT data was
located several degrees poleward of that obtained
from the IMAGE FUV SI12 instrument, suggesting electron precipitation poleward of the proton
aurora. In addition, a search for the location of
the east-west equivalent current reversal, known
E. E. Woodfield, et al., “Combining incoherent scat- as the Magnetic Convection Reversal Boundary
ter radar data and IRI-2007 to monitor the open-closed (MCRB), was made. The MCRB from the MIRfield line boundary during substorms”, J. Geophys. Res. ACLE magnetometer chain followed mainly the115, A00I15, doi:10.1029/2010JA015751
motion of the polar cap boundary during different substorm phases, but differences arose near
the Harang discontinuity.
intervals, it was found that the IRI-2007 method
produces an OCB proxy location which on average is 0.25◦ degrees equatorward (in AAGCM coordinates) of the boundary location produced by
the two-radar method. Comparing both methods
with OCB locations inferred from DMSP particle
data and IMAGE satellite data, they found thatboth methods performed quite well, and neither
method was particularly favoured over the other.
The magnitude of the mean offset to the IMAGE
OCB was found to vary between 0.1◦ and 2.7◦ inlatitude, depending on the event and the IMAGE
camera used.

Polar cap boundary location using IMAGE and EISCATThe ionospheric Polar Cap Boundary (PCB) can be
determined using different methods. In a studyof Hubert et al. (2010), electron temperatures fromO. Hubert, et al., “Comparison of the open-closed field
line boundary location inferred using IMAGE-FUV SI12
images and EISCAT radar observations”, Ann. Geophys. 28, 883–892, 2010.

21

Figure 26: (a) Keogram of SI12 counts along themeridian corresponding to the EISCAT field ofview on 22 September 2001. The overlaid whitesolid line represents the location of the EISCATPCB, the dotted lines show the SI12 PCB, and thered solid lines represent the MCRBs as determinedusing the MIRACLE magnetometer data. The vertical dashed line indicates the beginning of net flux
closure. (b) Blowup of the polar cap boundaries
determined during the interval with simultaneous
EISCAT observations, with the same line conventions as in panel (a).

Figure 27: Polar cap boundary detection using
the electron temperature as measured by EISCATVHF radar (top panel) and the CHAMP data of theelectron temperature and the field-aligned current
density (bottom panels). The vertical lines indicate the overpass of CHAMP and the EISCAT PCB
location.

Polar cap signatures
Detection of the Polar Cap Boundary (PCB) was
made by German EISCAT users in collaboration
with colleagues from Finland. Within the F region polar cap the electron temperature is reduced
compared to the surrounding auroral oval and thischange can be utilised to determine the polar cap
boundary. This method was tested by EISCAT andcoinciding satellite observations by CHAMP. The
increase in the electron temperature within in theauroral oval is generated by the collisional heating of the background plasma due to primary andsecondary electrons (Aikio et al. 2006). For polar cap identification, the variations of small-scale
Field-Aligned Currents (FAC) and electron temperatures as observed by CHAMP on polar passes
were used (Ritter et al. 2010). The PCB can be de22

tected clearly by a sudden drop of FAC density.
The found PCB latitude coincides very well withthe sharp electron temperature decrease that canbe observed by the EISCAT VHF radar, as shownin Fig. 27.
A. Aikio, et al., “Method to locate the polar cap boundary in the nightside ionosphere and application to a substorm event”, Ann. Geophys. 24, 1905-–1917, 2006.
P. Ritter, et al., “Signature of the polar cap in ionospheric currents and electron temperature as observedby CHAMP”, Poster at AGU 2010 Fall Meeting, San
Francisco, US, Dec. 13–17, 2010.
P. Ritter, et al., ”Signature of the polar cap in ionospheric currents and electron temperature as observedby CHAMP”, Poster at AEF Spring Meeting, Köln, Germany, Feb. 21–24, 2011.

Studies of particle precipitationand the aurora
Determination of the characteristic energy of precipitating electrons
Energetic electrons (tens to hundreds of keV)
deposit significant amounts of energy into the
D layer of the ionosphere. Riometers provide ameans of monitoring this electron precipitation bymeasuring the associated Cosmic Noise Absorption (CNA), but individually they are incapableof resolving the associated energy. However, thecombination of two imaging riometers with overlapping beams allows an estimate of the height ofpeak CNA, and hence the associated energy, to be
made. Wild et al. (2010) examined two methods
for estimating the height of CNA, using data from
two imaging riometers in northern Fennoscandia;
a 3-D reconstruction of CNA using Occam’s inversion and a technique based upon the triangulationof discrete absorption structures were developed.
The results of these methods were then comparedwith results from a previously published technique. It was found that, for these case studies, the height triangulation and 3-D reconstruction offered improvement over previous methods.
These techniques were tested using data from the
EISCAT VHF radar. The observations showed agood correlation between the estimates of peakheight of CNA from EISCAT and from the triangulation and 3-D reconstruction methods. Threecase studies were examined in detail — a slowly
varying absorption event, an afternoon spike, andan evening absorption spike event — and estimates of the characteristic energy of the precipitating particles were made. The substorm event
had a characteristic energy of ∼5 keV, whereas thecharacteristic energy for the morning event was
17-–20 keV. The analyses indicated that the afternoon spike event was the most energetic, having acharacteristic energy greater than 100 keV.
P. Wild, et al., “Triangulating the height of cosmic
noise absorption: A method for estimating the characteristic energy of precipitating electrons”, J. Geophys.
Res. 115, A12326, doi:10.1029/2010JA015766, 2010.

Figure 28: From top to bottom: (a) EISCAT Electron density. (log10 (m−3 )). (b) Absorption profile
using EISCAT electron density (dB/km). (c) Absorption in beam 9 of IRIS (solid line) and beam 656
of ARIES (dashed line) (dB). These beams intersect at 71 km. (d) Vertical absorption profiles using
the tomographic method (69.5◦ latitude, 19.2◦ longitude) with the peak height of CNA marked onin black from EISCAT. Error bars generated using
the length of the range gate. Height triangulation
method is marked in white (only cross-correlation
values over 0.6), 22 May 2008, 19:00–22:30 UT. Databetween 20:00 UT and 21:45 UT are not shown as
there was no activity.

tem, Auroral Structure and Kinetics (ASK), locatedat the EISCAT site in Tromsø. Short (1–2 s) periodsof flickering aurora were identified in which thefrequency of the brightness oscillations decreased
or increased smoothly over time. This study isbelieved to be the first detailed analysis of such“chirps”, or field-aligned bursts, in flickering aurora. The authors found that the electron precipitation energy was strongly anti-correlated withthe flickering frequency during all the identified
chirps. This result is consistent with the theory
that flickering aurora is caused by the resonanceinteraction between electromagnetic ion cyclotron
waves and precipitating electrons and that thewave parallel phase velocity is the primary factor
determining the electron acceleration produced bythis mechanism. The authors concluded that noother current theories could completely explainthese observations.
D. K. Whiter, et al., “Using multispectral optical observations to identify the acceleration mechanism responsible for flickering aurora”, J. Geophys. Res. 115, A12315,
doi:10.1029/2010JA015805, 2010.

Studies of dust and meteorites

Acceleration mechanism for flickering
auroraECOMA sounding rocket campaign
An analysis has been presented by Whiter et al.
(2010) of flickering (2–10 Hz) auroras observedwith a state-of-the-art multispectral imaging sys-

In 2010 extensive EISCAT measurements were performed by German scientists and connected to
the ECOMA-2010 sounding rocket campaign. The
23

This analysis is based on the detailed investigationof the spectral shape and the shape of the AutoCorrelation Function (ACF) as described by Rappet al. (2007) and Strelnikova and Rapp (2010).
Some initial results of the EISCAT VHF radar
data are shown in Fig. 30. The plot shows the estimated electron densities for the measurements.
Analysing the corresponding ACFs averaged over
the whole period with respect to the spectral
shape, the n parameter is less than 1 at altitudes
between 75 and 80 km, the altitude range where
meteor dust particles are expected. According to
the analysis by Strelnikova and Rapp (2010) the
fitting parameter n < 1 indicates the presenceof charged particles, in this case meteoric smoke
particles. Importantly, these preliminary n values
are in good agreement with initial results obtainedwith the particle detector on the ECOMA rockets.
M. Rapp, I. Strelnikova, and J. Gumbel (2007), “Meteoric smoke particles: Evidence from rocket andradar technique”, Adv. Space Res. 40, 809-–817,
doi:10.1016/j.asr.2006.11.021, 2007.

Figure 29: For each chirp, the first panels show
the detrended intensity time series from the ASK1(N2 or O+2 ) and ASK3 (OI) cameras. The second
and third panels show the power spectra obtained
from these time series for ASK1 and ASK3 respectively.

ECOMA (Existence and Charge state Of Meteoricsmoke particles in the middle Atmosphere) campaign was conducted at Andenes (Andøya Island,
Norway, 69◦ N, 16◦ E) in December 2010. During
this period a strong meteor shower, the Geminides, was approaching the Earth’s orbit and manymeteors were even visually observed. Three instrumented rockets were launched to investigate
meteoric smoke particles. The principle of the newrocket-borne ECOMA particle detector, which is
a combination between a classical Faraday cup
and Xenon flashlamps for active photoionizationof meteoric dust particles and their subsequent detection of corresponding photoelectrons, was introduced by Rapp and Strelnikova (2009). Detailed results of previous rocket launches werealready published by Rapp et al. (2010) whichclearly describes the instrumentation of the rocket
payload and the scientific results.
The ECOMA campaign was supported by several ground based instruments (mainly radars andlidars) near the rocket launch area as well as by
the EISCAT VHF radar. In summary, more than
80 hours of EISCAT radar observations were realised in the early morning hours, where the highest
number of meteors is detected. The backscatteredechoes from the EISCAT radar were analysed todetermine the spectral properties of these echoes.
24

M. Rapp, and I. Strelnikova, “Measurements of meteor smoke particles during the ECOMA-2006 campaign: 1. Particle detection by active photoionization”, J. Atmos. Solar-Terr. Phys. 71, 477-–485,
doi:10.1016/j.jastp.2008.07.011, 2010.
M. Rapp, et al., “Rocket-borne in situ measurements ofof meteor smoke: Charging properties and implications
for seasonal variations”, J. Geophys. Res. 115, D00I16,
doi:10.1029/2009JD012725, 2010.
I. Strelnikova, and M. Rapp, “Studies of polar mesosphere summer echoes with the EISCAT VHF andUHF radars: Information contained in the spectral shape”, Adv.
Space Res.
45, 247-–259,
doi:10.1016/j.asr.2009.09.007, 2010.

Solar wind studies
Interplanetary scintillation observations
A number of papers focusing on the use of EISCATinterplanetary scintillations (IPS) data appeared ina special issue of Solar Physics, resulting from aworkshop on the remote sensing of the inner heliosphere, held in Aberystwyth in 2009.
Bisi et al. (2010a) summarised results from ten
years of EISCAT observations of Stream Interaction Regions (SIRs) in the solar wind (1994
to 2003). Previous studies had shown that SIRs
were characterized by intermediate-velocity solar

Figure 30: Raw electron density observed on
Dec. 14th, 2010, with the EISCAT VHF radar (left).
From the analysis of the shape of the ACFs theaveraged fitting parameter n for the observational
period is determined (right). (Courtesy of G. Teiser,2011.)

wind and, in the case of compressive interactions, higher levels of scintillation. Bisi et al.
found that, after dismissing intermediate-velocity
observations associated with solar-wind transients(such as coronal mass ejections) the remaining intermediate velocities lay above coronal structures
where stream interaction would be expected. The
early stages of developing compression regions,on the leading edges of compressive stream interaction regions, were clearly detected as close
to the Sun as 30 R⊙ . The same approach wasapplied to study non-compressive interaction regions (shear layers) between solar-wind streams
of different velocities, where the stream interface
lay at near-constant latitude. The results confirmed that intermediate velocities seen in IPS
observations above stream boundaries may arise
from either compression regions, or from noncompressive shear layers. The variation in velocity was comparable in compressive and noncompressive regions — a result which may contain
important information on the geometry of developing SIRs. It is clear from these results that compressive and non-compressive interaction regions
belong to the same class of stream–stream interaction, with the dominant mode determined by thelatitudinal gradient of the stream interface.
Bisi et al. (2010b) reported results from a multiinstrument coordinated study of the solar eruptive event of 13 May 2005, discussing the resultant Earth-directed (halo) Coronal Mass Ejection(CME), and its effects on the terrestrial space environment and upper atmosphere. The Interplanetary CME (ICME) impacted the Earth’s magnetosphere and caused the most intense geomagnetic
storm of 2005, with a Disturbed Storm Time (Dst)index reaching -263 nT at its peak. The terrestrial

Figure 31: Observations of radio signals from EISCAT and MERLIN showing the anomalous signalstrength enhancement on 13 May 2005 due tothe flare/CME and associated coronal radio burst
overwhelming the IPS signal as taken from Jones etal. (2006). All EISCAT and MERLIN observations
were made at 1420 MHz with the exception of one(as marked in the figure).

environment responded to the storm on a global
scale. Combined observations from coronal andinterplanetary remote-sensing instruments, interplanetary and near-Earth in-situ measurements,
remote-sensing observations and in-situ measurements of the terrestrial magnetosphere and ionosphere, along with coronal and heliospheric modelling, were used to trace the origin, development,
propagation, terrestrial impact, and subsequentconsequences of this event, to obtain the mostcomprehensive view of a geo-effective solar eruption to date.
Bisi et al. (2010c) examined EISCAT data obtained during the April/May 2007 observing campaign to study the solar wind velocity structureduring the declining phase of Solar Cycle 23.
Many co-rotating and transient features were observed during this period. Tomographic reconstruction analysis was used to map the velocity
structure of the inner heliosphere and the resultscompared to a number of optical and other measurements made by spacecraft during this interval. The reconstructions showed clear co-rotating
regions during this period, and the time-series
extraction at spacecraft locations compared wellwith measurements made by the STEREO, Wind,
and ACE spacecraft. This was the first time thatsuch clear structures have been revealed using this
3D technique with EISCAT IPS data as input.
Dorrian et al. (2010) discussed the detection andevolution of a complex series of solar-wind struc25

Figure 33: Sample cross-correlation functions (topleft and right panels) from observations of IPS on
21 April 2007, one showing the appearance of anticorrelation (circled) near zero time lag, indicating the presence of magnetic field rotation in the
ray path. Each cross-correlation function is produced from a ten-minute data bin. Field rotations
are observed on timescales as short as 15 minutes,
suggesting structures with scale sizes of less than
400,000 km, placing them in the small-scale transient category. The bottom plot shows the variation in Vpos recorded over the course of the observing run (times indicate the start of each tenminute bin).

Figure 32: A set of four velocity 3D views showing the slow-wind portions of co-rotating structures at the dates and times shown (the highervelocity portions are not shown for clarity of viewing). These images form part of a movie (available online) covering this entire period. The Earthis shown as a blue sphere towards the bottom-leftof each image along with its orbital path shown inblack. The orange/red sphere in the centre of each
image represents the Sun (neither the Earth or the
Sun spheres are to scale).

sphere in the presence of two different solar windphenomena; a CIR and a CME. The CIR, detectedwith IPS and sampled in-situ at Venus, was foundtures in the days following the comet 2P/Encke to dramatically affect upstream solar wind conditail disconnection event in April 2007. EISCAT tions.
data were used to characterise the evolution ofJackson et al. (2010) reported the extension oftransient solar-wind structures ranging in size the UCSD three-dimensional tomographic techfrom <105 km to >106 km, and data from STE- nique for solar wind imaging, which already uses
REO were used to place them in context. One tran- input data from a range of in-situ and groundsient in the slow wind was observed being swept based instruments, including EISCAT. Their study
up and entrained by an SIR, which was later detec- examined the use of in-situ spacecraft data for conted in-situ at Venus by the ASPERA-4 instrument straining the time-dependent tomographic soluon VEX. This observation provides the first indic- tions. Jackson et al. demonstrated that, although
ation of heliocentric distances at which such tran- the largest effect on the reconstructions is seensients can become entrained. Dorrian et al. sug- close to the locations of the in-situ constraingested that the solar-wind transients may be the ing measurements, their inclusion significantly reinterplanetary counterparts of structures reported duces the error of the global 3D reconstruction.
from coronagraph observations and the transient The effect is to improve the real-time measuring
magnetic structures reported from in-situ meas- technique, as well as to enable more accurate foreurements in interplanetary space.
casting.
Whitaker et al. (2010) reported the first combination of IPS data with in-situ plasma measure- M. M. Bisi, et al., “Interplanetary Scintillation Observaments from Venus Express. The ion mass ana- tions of Stream Interaction Regions in the Solar Wind”,
lyser instrument on VEX was used to investigate Solar Physics 261(1), 149–172, DOI: 10.1007/s11207-009solar wind interaction with the Venusian magneto- 9471-1, 2010a.
26

M. M. Bisi, et al., “From the Sun to the Earth: the 13 May
2005 Coronal Mass Ejection”, Solar Physics 265(1-2), 49–
127, DOI: 10.1007/s11207-010-9602-8, 2010b.
M. M. Bisi, et al., “Three-Dimensional (3-D) Reconstructions of EISCAT IPS Velocity Data in the Declining Phaseof Solar Cycle 23”, Solar Physics 265(1–2), 233–244, DOI:
10.1007/s11207-010-9594-4, 2010c.
G. D. Dorrian, et al., “Transient structures and stream
interaction regions in the solar wind: Results from EISCAT interplanetary scintillation, STEREO HI and Venus
Express ASPERA-4 observations”, Solar Physics 265(12), 207–231, DOI: 10.1007/s11207-010-9599-z, 2010.
B. V. Jackson, et al., “Inclusion of in-situ measurements
into the UCSD time-dependent tomography to constrain and better forecast remote-sensing observations”,
Solar Physics 265, 245–256, 2010.

Figure 34: The critical index of refraction, nx andthe parameter lx , are plotted for a succession ofrays in the meridional plane. The values of nx
and lx are taken at the point of closest approachto the plasma resonance. The ionosphere has a
3% density reduction close to the magnetic zenith.
The long black
p line represents the radio window at
nx = −lx Y /(1 + Y ). The colour indicates thetransmission factor, which reaches 1 at the radio
window. The curve returns to the black line in theupper left corner of the figure, as rays propagatingin the duct reach the radio window and are transmitted.

I. C. Whitaker, et al., “In-situ observations of a corotating interaction region at Venus identified by IPS
and STEREO”, Solar Physics 265, 197–206, 2010.

Studies of fundamental plasma
physics
Ray tracing analysis of L mode pumpingof the ionosphere

metic has been used to fit the incoherent scatter
spectra at 100 km altitude measured by EISCAT
UHF during the ionospheric heating campaign
operated in X-mode at 10:08, 10:16, 10:24, 10:40,
10:56 UT and in O-mode at 10:32 and 10:48 UT
on January 11th, 2008. The measured incoherent scatter spectra of these seven heating cases
and a comparison between fitting results of GUISDAP and the super-Gaussian model is shown in
Fig. 35. GUISDAP uses two assumptions, thatis that the ionosphere plasma is in equilibrium
and that the electron and ion temperature ratio isconstant. This may bring some errors when fitting results. Particularly, when the pumping isin X-mode, the fitting results of GUISDAP will
be much higher than the measured ones. By usE. Nordblad, and T. B. Leyser, “Ray tracing analysis of L ing the super-Gaussian model with the introducmode pumping of the ionosphere, with implications for tion of independent electron temperature and nonthe magnetic zenith effect”, Ann. Geophys. 28, 1749– Maxwellian index, however, a better fitting result
1759, doi:10.5194/angeo-28-1749-2010, 2010.
can be achieved. Furthermore, the peak power in
O-mode at 10:32 and 10:48 UT respectively is obviObservations of heating experiments in ously higher than that of the four X-mode heating
at 10:08, 10:24, 10:40 and 10:56 UT.
the low ionosphere in polar winterThe “magnetic zenith effect” had first been observed with the Heater several years ago as anincreased plasma response to Ordinary (O) mode
pump waves and optical emissions around theMagnetic Zenith (MZ). Using ray tracing of ordinary mode HF waves in an ionosphere withkilometre-scale field aligned density depletions,or ducts, Nordblad and Leyser (2010) have now
found that transmission across the plasma resonance becomes possible at new locations as rays are
guided into the so-called L mode (Fig. 34. Stronger
transmitted fields are seen in some directions, notably at inclinations close to the vertical or the MZ.
It is argued that the results could have implications for the MZ.

Based on super-Gaussian incoherent scatter theoretical model, the LM (Levenberg-Marquart) arith-

X. Bin, et al., “Observations of the heating experimentsin the polar winter ionosphere — Analysis in low re-27

to the south of zenith, thus allowing HF pumping in the field-aligned direction (magnetic zenith,
MZ). In the course of the experiments the heating facility was operating at 3.95, 4.04, 4.9128,
and 5.423 MHz, with X-mode polarization, andwith 10 min continuous HF pulses. The experiments were carried out during quiet magnetic conditions.
The modified ionospheric F region was probed
by the CUTLASS Hankasalmi, Finland radar(63◦ N, 27◦ E). The CUTLASS (Finland) radar transmitter site is located approximately 1000 km southof the Tromsø heating facility. In the course ofexperiments the CUTLASS radar was running a
Figure 35: The measured and fitted power spectral
non-standard mode optimised for observation ofdensities of the seven heating cases (dots: measheating effects over Tromsø with one fixed beam
ured data; dash-dotted line: fit results of GUIS(beam 5) with a high temporal and spatial resolDAP; solid line: fit results of the super-Gaussianmodel).
ution. It operated almost simultaneously at several frequencies from ∼10 to 17 MHz and wastherefore sensitive to AFAIs with the spatial sizegion”, Chinese Journal Geophysics 53, 1263–1268, (in across the geomagnetic field of the order of l⊥ ≈Chinese) 2010.
15 − −9 m respectively. The HF heating facility
at Tromsø is located adjacent to the EISCAT UHF
Activities by the Arctic and Antarctic Re- incoherent radar (930 MHz). During the experiments the UHF radar measured the ionosphericsearch Institute (AARI) in 2010
plasma parameters in the direction of the magnetic
Two extensive HF heating campaigns were held by zenith. Ionograms, taken every four minutes usthe Arctic and Antarctic Research Institute (AARI), ing the EISCAT ionosonde (dynasonde), indicatedRussia, in March and November 2010 in a close a smooth F2 layer with the critical frequency foF2
collaboration with the Leicester University (Prof. below the heater frequency, fH , by 0.4–0.6 MHz.
T. Yeoman) related to studies of small-scale ar- At the same time the heater frequency was neartificial field-aligned irregularities (AFAIs) in the or just below the extraordinary mode critical freF-region of the ionosphere under X-mode heat- quency (fxF2 ). Therefore, it was suggested that theing. It is well known that AFAIs occur at the up- HF pump wave with X-mode polarisation was reper hybrid resonance altitude due to the thermal flected from the ionosphere. Figure 36 shows theparametric (resonance) instability when ordinary CUTLASS Hankasalmi backscatter power during(O-mode) polarised HF pump waves reach the the experiment on 6 March 2010.
ionospheric reflection height. Since the resonance
Before the X-mode heating, the HF pump wave
altitude in the ionosphere cannot be reached by with O-mode polarisation was radiated for thean extraordinary polarisation (X-mode) HF pump first two heater-on periods. It is seen from Figwave, only O-mode waves can excite AFAIs. The ure 36 that the intense signals scattered fromresults obtained clearly demonstrate that the X- AFAIs, excited by the HF pump wave with Omode HF pump wave, radiated into the magnetic mode polarisation, were observed at three CUTzenith from the EISCAT/Heating facility, can also LASS frequencies in the heater-on period fromgenerate very strong AFAIs in the high-latitude F- 15:26–15:36 UT, when the electron density inregion ionosphere when the heater frequency is the F region dropped, and the heater frequency,
above foF2 but comparable to the extraordinary fH = 4.9128 MHz, was near and then slightly
mode critical frequency, fxF2 ≈ fH > foF2 .
above the critical frequency of F2 layer, foF2 =The experiments were carried out on 5, 6 and 4.7 − −4.9 MHz. During the heater-on period
8 March 2010 and on 4, 5, 6, 7 and 10 Novem- from 15:41–15:51 UT the values of foF2 becameber 2010. The EISCAT HF heating facility (69.6◦ N, ∼4.4 MHz and the signals scattered from AFAIs
19.2◦ E; magnetic dip angle I = 78◦ ) was used to disappeared at 17 MHz. At 10 and 13 MHz themodify the ionosphere in the high-latitude F re- weak scattered signals were observed during thegion. The HF heater antenna beam was tilted 12◦ first 3–4 minutes of the 10 min heating cycle and28

Figure 37: Backscattered power from the Hankasalmi (Finland) CUTLASS radar (beam 5) at operational frequencies of about 10, 11.5 and 13 MHz
in the range-gate – universal time UT coordinates
for contrasting O/X-mode heating on 6 November 2010 between 13:30 and 15:00 UT. O/X-mode
heater-on periods are marked in the time axis.

Figure 36: Backscattered power from the Hankasalmi (Finland) CUTLASS radar (beam 5) at operational frequencies of about 10, 13 and 17 MHz forcontrasting O/X-mode heating on 6 March 2010
between 15:20 and 17:00 UT. The behaviour ofthe backscattered power at every operational frequency averaged over three 15 km gates, corresponding to the central part of the heated beam
is shown in the top panel and their behaviour inthe range-gate – universal time UT coordinates are
given in the bottom panels. O/X-mode heater-on
periods are marked in the time axis.

then disappeared. The polarisation of the HF
pump wave was changed from O to X-mode in
the next heater-on period from 15.56–16.06 UT.
The polarisation change of the heater wave produced scattered signals over Tromsø at three CUTLASS frequencies. On 6 March 2010, X-mode heating was performed during three consecutive heating cycles. The distinctive features of X-mode
AFAIs with different spatial size across the geomagnetic field are clearly seen from the behaviourof the backscattered power at every operationalfrequency averaged over three 15 km gates, corresponding to the central part of the heated beam (seethe top panel in Figure 36). The excitation of AFAIs

with l⊥ ≈ 11 m, responsible for the CUTLASS
backscatter, occurred in all three heater-on periods. They appeared within a time interval from10 s to 3 minutes after the heater was turned on.
Their decay time was approximately 6 and 15 minafter the first and second X-mode cycle respectively.
The results of the experimental observations on
5 March 2010 are very similar to the case of 6
March 2010 but in this experiment only AFAIs
with l⊥ ≈ 15, 11, and 9 m were excited. In thecourse of the experiment on 8 March 2010 the HF
pump wave was radiated at frequency of fH =5.423 MHz. It was the only experiment when Omode heating at the same frequency was not carried out prior to the X-mode heating. Nonethelessduring the experiment on 8 March 2010 the AFAIs
with different spatial sizes of l⊥ ≈ 15, 11 and 9 m
were excited in four consecutive 10 min heater-on
periods.
A very similar behaviour of AFAIs in the F region of the ionosphere excited by HF pump wave
with X-mode of polarisation was observed duringexperiments on November 2010. Figure 37 shows
the CUTLASS Hankasalmi backscatter power during the experiment on 6 November 2010.
EISCAT UHF incoherent scatter data from
Tromsø site, obtained in the direction of themagnetic zenith, were examined to estimate thechanges in the electron temperature (Te ) and electron density (Ne ) at different altitudes, accompa29

nying the generation of AFAIs induced by thepowerful HF radio waves with X-mode polarization. The results obtained for contrasting O/Xmode heating clearly demonstrate that an HF
pump wave with X-mode polarization heats theionosphere through collision processes more effectively than an O-mode HF heater wave. This
is in agreement with the recent results of Gustavsson et al. (2010) who showed that heating of
ionospheric electrons is more efficient for X-mode
heating than for O-mode heating. In our experiments the Te enhancements under X-mode heating
reached values of ∼ 50%, above the backgroundlevel over an altitude range from 186 to 247 km.
Temporal variations of Te with 30 s integration
time at different altitudes in the direction of themagnetic zenith during the experiment on 6 March2010 are plotted in Fig. 38. As was also shown in
Fig. 36, weak scattered signals were observed at
10 and 13 MHz during the O-mode heating cyclefrom 15:41–15:51 UT. Therefore not only the pureohmic heating was observed here. During the next
three consecutive X-mode heating cycles Te enhancements of up to 50% above the backgroundlevel occurred. The strongest Te enhancements
took place at 214 km from 16:16–16:26 UT cycle.
The electron density behaviour in the magnetic
zenith (Fig. 39) shows some interesting features.
It is seen that Ne increased by up to 30% above
the background level at an altitude of 282 km during the X-mode heating cycles. Ne enhancements
were also observed at 246 km, however no significant enhancements were observed at 214 km
where the strongest Te enhancements occurred.
The total electron content along magnetic field line
was calculated in the altitude range from 185 to
325 km and its behaviour is also shown in Fig. 39(top panel). The well-defined increases are clearlyseen in the total electron content from the 15:56–
16.06 and 16:16–16:26 UT heater-on cycles. Suchelectron density enhancements can be attributed
to HF-induced ionization production rather thanthe change of the density distribution due to thethermal diffusion. Note that the experiment was
conducted under quiet magnetic conditions, thus
any Ne increases due to soft electron precipitationfrom the magnetosphere could be excluded.
Worth mentioning is that the incoherent backscatter spectra obtained with the EISCAT UHF
radar during X-mode HF pumping demonstratestrongly heater-enhanced ion line shoulders andplasma lines, which are unusual for X-mode heating. The heater-enhanced ion and plasma lines
are due to the electromagnetic parametric de30

Figure 38: Variations in time of the electron temperature Te with error-bars at different altitudes (toppanel) and its behaviour in the altitude – universal time UT coordinates (bottom panel), obtained
from the EISCAT UHF radar observations for contrasting O/X-mode heating on 6 March 2010 from
15:38–17:00 UT. O/X-mode heater-on periods aremarked in the time axis.

cay instability (Stubbe, 1996). Behaviour of thedownshifted, unshifted, and upshifted ion line
amplitudes in the course of the experiment on
6 November 2010 is shown in Figure 40.
The mechanism of the X-mode AFAIs is notclear. Vas’kov and Ryabova (1998) have theoretically shown that the generation process of shortwavelength (upper-hybrid and electron cyclotron)
plasma oscillations can be produced by induced
scattering of a powerful extraordinary HF radio
waves by ions. They also note that the high frequency turbulence excited near the reflection levelof the powerful extraordinary HF wave leads tothe substantial enhancements of low frequency
plasma perturbations. The large growth and decay times observed are typical for large-scale ionospheric irregularities with spatial scales of the order of the heated patch (∼60 km). In such acase one would expect that the behaviour of thesmall-scale AFAIs, with spatial scales of the order l⊥ ≈ 9–15 m, which are responsible for thestrong backscattered signals from the CUTLASS
measurements, is driven by the large-scale ionospheric irregularities.

Results and future plans”, Problems of Arctica and Antarctica 84, 81–99, (in Russian) 2010.
N. F. Blagoveshchenskaya, et al., “Phenomena in thehigh latitude ionosphere induced by powerful HF radio
waves from EISCAT/Heating facility: Part 1. Peculiarities of excitation and behavior of small-scale artificial
field-aligned irregularities and ionospheric plasma features”, Radiophysics & Quant. Electr. 53, 9–10. 2010.
N. F. Blagoveshchenskaya, et al., “Results from Russian
experiments on the impact of powerful HF radio waves
in the high latitude ionosphere by using EISCAT facilities”, Solar-Terrestr. Physics, (in press), (in Russian)
2010.
N. F. Blagoveshchenskaya, et al., “Artificial small-scale
field-aligned irregularities in the high latitude F regionof the ionosphere induced by an X-mode HF heaterwave”, Geophys. Res. Lett., doi:10.1029/2011GL046724,
in press, 2011.
Figure 39: Variations in time of the electron density Ne with error-bars at different altitudes and thetotal electron content in the altitude range from180 to 325 km (top panel) and the Ne behaviour inthe altitude – universal time UT coordinates (bottom panel), obtained from the EISCAT UHF radarobservations for contrasting O/X-mode heating on
6 March, 2010 from 15:38–17:00 UT. O/X-mode
heater-on periods are marked in the time axis.

UK studies involving artificial heating

Gustavsson et al. (2010) presented electron temperature variations during an EISCAT experimentwhen the HF heater was transmitting at frequencies above the peak ionospheric critical frequency.
During these HF transmission periods, the electron temperature increased from 2000 K up to2800 K, and both pump frequency and the polarisation were altered between the pump pulses.
The observed temperature variation was compared with numerical solutions to the electron energy equation with ohmic heating, modelling theeffect of the radio wave heating on the plasma.
The agreement between the observations and themodel was found to be good.
Kosch et al. (2010) also studied an interval
where HF heating caused strong increases in electron temperature, in this case accompanied byartificially induced ion upwelling. The pumpenhanced electron temperatures reached up to∼4000 K at altitudes above 350 km, and ion upwelling reached up to ∼300 m/s above 500 km
altitude. The authors concluded that the pumpinduced electron pressure gradient could explain
Figure 40: Behaviour of the downshifted, unthe ion velocity below 450 km. Between 450 andshifted, and upshifted ion line amplitudes in the
600 km the electron pressure gradient was foundcourse of the experiment on 6 November 2010 fromto correlate equally with ion acceleration and ion
13:45 to 14:35 UT. HF heating with X-mode of povelocity, representing the transition altitude to freelarization was made from 13:50–14:00, 14:05–14:15,
ion acceleration. The electron gas pressure gradiand 14:20–14:30 UT.
ent was strong enough to explain ion upwelling,at least up to 600 km altitude. Kosch et al also
N. F. Blagoveshchenskaya,“Phenomena initiated by pointed out that such types of active experiments
powerful HF radio waves the high latitude‘ionosphere: provide the possibility to estimate the variation
31

Figure 41: (a) The observed Te variations agree
well with the solution to the electron energy equation with ohmic heating by the HF pump wave; (b)both the temporal characteristics and the variation
between different HF pulses, where the pump frequency, power, and polarization varied. (c) It isclearly seen that the only pulse where there is asignificant discrepancy between observations (bluecurve) and modelling (red curve) results is the firstpump period. For this transmission period it islikely that the transmitted frequency was just at or
below the X-mode critical frequency, leading to reflection of the pump wave.

Figure 42: Field-aligned EISCAT UHF radar datafor 17—20 UT on 6 October 1998. From top tobottom, the panels show electron density, electron
temperature, ion temperature, and ion velocity
between 100 and 600 km altitude. The “noisy data”
in each panel below ∼350 km correspond to thepump-induced ion line overshoot phenomenon.

of the F layer ion-neutral collision frequency andneutral density with altitude from ground-based
observations.
Vickers et al. (2010) presented a study of thespectral features in incoherent scatter data causedby the Purely Growing Mode (PGM), during thefirst few seconds of EISCAT heating experiments.
These features, often referred to as “overshoot” effects, are indicators of turbulent non-Maxwellian
plasma, and the analysis of the affected spectra using standard incoherent scatter data analysis software leads to a poor estimation of the plasma
parameters, particularly for electron and ion temperature. In this study, the authors developed aprocedure to derive a more reliable estimate ofplasma temperature during periods when the incoherent scatter spectrum is affected by contamination from the PGM. This was achieved by re32

moving the PGM from the measured spectrum
and then analysing the modified spectrum using standard software. The results were thencompared to those obtained from the analysis of
the original, contaminated spectra. It was foundthat the differences between the results obtained
from the corrected and uncorrected spectra werestrongly proportional to the magnitude of the
PGM feature. Vickers et al. also showed that thebulk temperatures during the remainder of the“heater on” period (after the overshoot) could generally be estimated reliably by the standard analysis software, though with some important exceptions. These results are important since theplasma temperatures play a crucial role in governing thermal conduction processes, and their correct estimation is thus very important to understanding the underlying physical processes which
occur during ionospheric heating.

Figure 43: Spectrum correction results for the spectrum at 209 km, at 12:55 UT on 7 October 1997.
(a) The measured ion acoustic spectrum (blue) andthe a priori theoretical spectrum (green). (b) The
measured spectrum (blue) and best fitted Gaussian
peak. (c) The fitted theoretical spectrum (green)
and the best fit corrected spectrum (blue). (d) The
measured ACF (green) and the ACF that resultsfrom the Fourier transform of the best fit corrected
spectrum.

Radio heating of the free electrons in the mesosphere is an important diagnostic technique forthe phenomenon of Polar Mesosphere Summer
echoes (PMSE). Due to a lack of suitable observations, the heating must be modelled when studying its effect on PMSE. In order to try to validate
these models, Senior et al (2010) implemented across-modulation technique on the Tromsø Heater,
to compare the absorption of a diagnostic radio
wave in the heated and unheated plasma. The results were compared to predictions from a model
similar to that used for estimating the heating in
PMSE studies. It was found that, after allowing for
certain instrumental effects, the model overestimated the change in the absorption of the diagnostic
wave by a factor of 1.5–2.5. The authors suggested that the assumption that the electron distribution function remains Maxwellian during heating
could contribute to this discrepancy.
Shergill et al. (2010) reported a statistical studyof intensity distributions in patches of plasma
density irregularities excited by the Tromsø heater
during beam-sweeping experiments, and detected by the CUTLASS radar in Finland. During these experiments, the heater beam direction
was steadily changed from northward to southward pointing. Comparisons were made between
the statistical parameters of the CUTLASS backs-

Figure 44: Comparison of observations and modeling for (left) Case 1 and (right) Case 2. The thingray lines are the diagnostic absorption change
profiles for each 60 s sounding. The heavy blackline is the median of these profiles; refer to thelower scale. The heavy dashed line is the modelleddiagnostic absorption change profile; refer to theupper scale.

catter power distributions and modelled heater
beam power distributions. Despite the sometimes seemingly unpredictable nature of the unaveraged results, good agreement was observed
between the statistical parameters and the modelled beam, clearly indicating the direct causal
connection between the heater beam and the irregularities. The results also gave compelling evidence in support of the upper hybrid theory of irregularity excitation.
B. Gustavsson, et al., “The Rise and Fall of Electron
Temperatures I: Ohmic Heating of Ionospheric Electrons
from Under-Dense HF-radio Wave Pumping”, J. Geophys. Res. 115, A12332, doi:10.1029/2010JA015873,
2010.
M. J. Kosch, et al., “An analysis of pump-induced artificial ionospheric ion upwelling at EISCAT”, J. Geophys.
Res. 115, A00I12, doi:10.1029/2010JA015854, 2010.
A. Senior, et al., “Diagnosing Radio Plasma Heating in
the Polar Summer Mesosphere using Cross-Modulation:
Theory and Observations”, J. Geophys. Res. 115,
A09318, doi:10.1029/2010JA015379, 2010.
H. Shergill, et al., “A statistical study of the spatial distribution of Cooperative UK Twin Located Auroral Sounding System (CUTLASS) backscatter power during EISCAT heater beamsweeping experiments”, J. Geophys.,Res. 115, A05307, doi:10.1029/2009JA014659, 2010.
H. Vickers, et al., “A method for improving plasma temperature estimates from incoherent scatter analysis during artificial ionospheric modification experiments”, J.
Geophys. Res. 115, A11316, doi:10.1029/2010JA015606,
2010.

33

Figure 46: Measurement results of incoherent scatter spectra.

Figure 47: Electron temperature and density during the HF modification experiment (HF off –white; HF on – black: Maxwellian; gray: the irregularities model).

Figure 45: Variation of the statistical parameters of
CUTLASS data measured during beam-sweeping
run A. Vertical lines indicate the beginning of each
sweep, and the horizontal dashed line in panel drepresents the upper hybrid width. The horisontal
line in panel a indicates the position verticallyabove the heater.

Inversion results of incoherent scatter
spectraUsing powerful HF wave injection the equilibrium of the ionospheric plasma will be modified,that is a non-Maxwellian particle velocity distribution can be produced. The effects of the nonMaxwellian factors and plasma parameters on the
spectra characteristics are overlapped and complicated. The ion line spectra near 186 km altitude
measured by EISCAT UHF from 9:38 to 11:14 on
August 15th 2006, are shown in Fig. 46. The heater
was operated at 4.544 MHz, O-mode with a modulation cycle of 4 min on followed by 4 min off
and zenith angle 12◦ (geomagnetic field). Except
for a bad data point at 10:54, the incoherent scatter spectra descend, whereas the peak-to-valley ratio of the spectrum line increases during heating.
Either the increase of the electron temperature andthe non-Maxwellian indices or the decreases of theelectron density and ion temperature can result
34

in these modifications. Consequently, the plasma
parameters obtained by fitting experimental spectra with the Maxwellian distribution, may be affected.
As shown in Fig. 47, the electron temperature
increases up to 27% (627 K), whereas the modification of electron density is very faint. When theheater is on, the electron temperature still clearly
increased, but the incremental amplitude is lower
than that obtained from standard analysis methods. The standard analysis procedure also overestimate the electron density, which may result incompletely erroneous conclusions. In most cases,
the reduction of the electron density can be seen in
the inversion results from the irregularities model,
which is consistent with the prediction of the theoretical model, whereas the phenomenon does notappear in the Maxwellian analysis results.

B. Xu, et al., “The inversion of incoherent scatter spectrawith a non-Maxwellian electron distribution”, J. Atmos.
Terr. Phys. 72, 492–497, 2010.

Spectra of non-Maxwellian distributions
The equilibrium of the ionospheric plasma is modified when using powerful HF wave injection, sothat a non-Maxwellian particle velocity distribution may be produced. The non-Maxwellian electron distribution can be described by a superposition of a high temperature distribution and a background distribution
1−RR2
exp(−v 2 /a2 ) + 1/2
exp(−v 2 /vth),
π 1/2 aπ vth(1)pwhere a = 2kB Te /me denotes the thermal velocity of the background electrons, and R the electron density ratio of the high temperature component and the background, Te the backgroundelectrons temperature, me the pelectron mass, kB
Te /Te the irregthe Boltzmann constant, m =ularities temperature coefficient and vth = ma.
By neglecting the magnetic field and collisions,the power spectra are given byfe = ω  2πZ G 2  ω 
e
fi
+
k
k
ε
k
(2)
where k is the wave vector, Z the charge numberof the ions, ε = 1+Gε e+Gε i the dielectric function,
and Ge and Gi are defined respectively asZ ∞4πe2 ne0 k × ∂fe /∂v
dv
Ge (k, ω) =(3)
2
me k Bω−k×v−∞
Z ∞4πe2 ni0 k × ∂fi /∂v(4)dv
Gi (k, ω) =2
mi k B
ω−k×v−∞
S(k, ω) =

Ge
2π
1−
k
ε

Figure 48: Variation of ISR spectra having nonMaxwellian indices.

New radar techniques2

fewhere fe is given by Eq. (1).
The effects of the ordinary ionosphere parameters and the non-Maxwellian indices on the incoherent scatter spectra are presented in Fig. 48.
With the increase in the electron temperature, theion resonance frequency increases and the peakto-valley ratio in the spectrum enhances. With
the increase in the ion temperature, however,the peak-to-valley ratio declines, and the spectral
width is broadened. The ion resonance frequency
and the area increase and the spectral peak becomes sharper as electron density increases. With
increase in R, the amplitude of the ion line and thespectral area is reduced while the peak-to-valley
ratio enhances. It is clear that effects from the nonMaxwellian factors and from the plasma parameters on the spectra characteristics overlap.
B. Xu, et al., “The inversion of incoherent scatter spectrawith a non-Maxwellian electron distribution”, J. Atmos.
Terr. Phys. 72, 492–497, 2010.

Simulation of post-ADC digital beamforming for large aperture array radars
The feasibility of using a Fractional Sample Delay(FSD) system in the planned EISCAT_3D incoherent scatter radar has been simulated. Key requirements include a frequency-independent beam direction over a 30 MHz band centered around
220 MHz, with correct reconstruction of pulse
lengths down to 200 ns. The clock jitter fromsample to sample must be extremely low for the
integer sample delays. The FSD must also be able
to delay the 30 MHz wide signal band by 1/1024thof a sample without introducing phase shifts, andit must operate entirely in baseband. An extensive simulation system based on mathematical models has been developed, with inclusionof performance-degrading aspects such as noise,timing error, and bandwidth. Finite Impulse Response (FIR) filters in the baseband of a bandpass-sampled signal are used to apply true timedelay beamforming. It has been confirmed thatsuch use is both possible and well behaved. The
target beam-pointing accuracy of 0.06◦ is achievable using optimized FIR filters with lengths of
36 taps and an 18 bit coefficient resolution (Fig. 49).
Even though the minimum fractional delay stepnecessary for beamforming is ∼13.1 ps, the maximum sampling timing error allowed in the arrayis found to be σ ≤ 120 ps if the errors are close tostatistically independent.

35

Figure 49: A beam width test run is shown for
the 12×4 test array with 120 ps timing error included. The 0.06◦ maximum beam width demandis met only for elevations above ∼20◦ . There arebarely visible peaks that show the limited but existent effect of a distributed timing error on the beamwidth.
G. Johansson, et al., “Simulation of post-ADC digital
beamforming for large aperture array radars”, Radio
Sci. 45, RS3001, doi:10.1029/2008RS004124, 2010.

36

List of publications 2010
Aruliah, A.L., E.M. Griffin, H.-C. I. Yiu, I. McWhirter,and A. Charalambous, SCANDI an all-sky Doppler imager for studies of thermospheric spatial structure, Ann.
Geophys., 28, 549-567, 2010.
Bin, X., Zhange Wang, Kue Xue, Jian Wu, Zhensen Wu,
Jun Wu, Yubo Yan, The inversion of incoherent scatter spectra with a non-Maxwellian electron distribution,
Journal of Atmospheric and Solar-Terrestrial Physics,
72, 5-6, 492-497, doi:10.1016/j.jastp.2010.01.006, 2010.
Bisi, M.M., R.A. Fallows, A.R. Breen and I.J. O’Neill, Interplanetary Scintillation Observations of Stream Interaction Regions in the Solar Wind, Solar Physics, 261,1,
149-172, DOI: 10.1007/s11207-009-9471-1, 2010.
Bisi, M.M., A.R. Breen, B.V. Jackson, R.A. Fallows, A.P.
Walsh, Z. Mikic, P. Riley, C.J. Owen, A. GonzalezEsparza, E. Aguilar-Rodriguez, H. Morgan, E.A. Jensen,
A.G. Wood, M. Tokumaru, P.K. Manoharan, I.V.
Chashei, A.S. Giunta, J.A. Linker, V.I. Shishov, S.A.
Tyul’bashev, G. Agalya, S.K. Glubokova, M.S. Hamilton,
K. Fujiki, P.P. Hick, J.M. Clover, and B. Pinter, From the
Sun to the Earth: the 13 May 2005 Coronal Mass Ejection,
Solar Physics, 265, 1-2, 49-127, DOI: 10.1007/s11207-0109602-8, 2010.
Bisi, M.M., B.V. Jackson, A.R. Breen, G.D. Dorrian, R.A.
Fallows, J.M. Clover and P.P. Hick, Three-Dimensional(3-D) Reconstructions of EISCAT IPS Velocity Data in
the Declining Phase of Solar Cycle 23, Solar Physics, 265,1-2, 233-244, DOI: 10.1007/s11207-010-9594-4 , 2010.
Blagoveshchenskaya N.F., Phenomena initiated bypowerful HF radio waves the high latitude ionosphere:
Results and future plans. Problems of Arctica and Antarctica, V.84. N1, pp. 81-99., (in Russian), 2010.
Blagoveshchenskaya, N.F., T.D. Borisova, M.T. Rietveld,
T.K. Yeoman, D.M. Wright, M. Rother, H. Lühr, E.V.
Mishin, C. Roth, Results from Russian experiments on
the impact of powerful HF radio waves in the highlatitude ionosphere by using EISCAT facilities, SolarTerrestr. Physics, (in Russian), (in press) 2010.
Blagoveshchenskaya N.F., T.D. Borisova, T.K. Yeoman, M.T. Rietveld, Modification of the high latitude ionosphere by powerful HF radio waves. 1.

Results from multi-instrument ground-based observations, Radiophys. & Quant. Electr., 53, 9-10, 512-531,
DOI: 10.1007/s11141-011-9247-y , 2011. (Translated from
Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika,
53, 9-10, pp. 571-593, September-October 2010.)
Blelly, P.-L., D. Alcayde, and A.P. van Eyken, A new
analysis method for determining polar ionosphere andupper atmosphere characteristics from ESR data: Illustration with IPY period, J. Geophys. Res., 115, A09322,
doi:10.1029/2009JA014876, 2010.
Brosch, N., I. Häggström, A. Pellinen-Wannberg, and A.
Westman, Unusual features in high statistics radar meteor studies at EISCAT, Monthly Notices of Royal Astronomical Society, 401, 2, 1069-1079, 2010.
Dahlgren, Hanna, Multi-spectral analysis of fine scaleaurora, PhD thesis, University of , Sweden, 2010.
Dorrian, G.D., A.R. Breen, J.A. Davies, A.P. Rouillard,
I.C. Whittaker, C.J. Davis, D.S. Brown, R.A. Fallows,
R.A. Harrison and M. Grande, Transient structures andstream interaction regions in the solar wind: Resultsfrom EISCAT interplanetary scintillation, STEREO HI
and Venus Express ASPERA-4 observations, Solar Physics, 265, 1-2, 207-231, DOI: 10.1007/s11207-010-9599-z,
2010.
Gillies, R.G., G.C. Hussey, G.J. Sofko, D.M. Wright, J.A.
Davies, A comparison of EISCAT and SuperDARN Fregion measurements with consideration of the refractive index in the scattering volume, J. Geophys. Res., 115,
A06319, doi:10.1029/2009JA014694, 2010.
Grydeland, T., and C. La Hoz, Phase calibration of aradar interferometer by means of incoherent scattering,
Radio Sci., 45, RS4001, doi:10.1029/2009RS004249, 2010.
Gustavsson, B., M. T. Rietveld, N. V. Ivchenko, and M.
J. Kosch, The Rise and Fall of Electron Temperatures I:
Ohmic Heating of Ionospheric Electrons from UnderDense HF-radio Wave Pumping, J. Geophys. Res.,115,
A12332, doi:10.1029/2010JA015873, , 2010.
Hosokawa, K., Y. Ogawa, A. Kadokura, H. Miyaoka,
and N. Sato, Modulation of ionospheric conductanceand electric field associated with pulsating aurora, J.
Geophys. Res., 115, A03201, doi:10.1029/2009JA014683,
2010.

37

Hubert, B., A. T. Aikio, O. Amm, T. Pitkänen, K.
Kauristie, S. E. Milan, S. W. H. Cowley, and J.-C. Gérard,
Comparison of the open-closed field line boundary location inferred using IMAGE-FUV SI12 images and EISCAT radar observations, Ann. Geophys., 28, 883-892,
2010.
Johansson, G., J. Borg, J. Johansson, M. Lundberg Nordenvaad, and G. Wannberg, Simulation of post-ADC digital beamforming for large
aperture array radars, Radio Sci., 45, RS3001,
doi:10.1029/2008RS004124, 2010.
Kosch, M.J., Y. Ogawa, M.T. Rietveld, S. Nozawa andR. Fujii, An analysis of pump-induced artificial ionospheric ion upwelling at EISCAT, J. Geophys., 115,
A12317, doi:10.1029/2010JA015854, 2010.
Li, Hailong , Jian Wu, Jiying Huang, Maoyan Wang, Reflection characteristics of layered media in polar mesopause occurring polar mesosphere summer echoes,
Plasma Science and Technology, 12, 4, 416-420, doi:
10.1088/1009-0630/12/4/07, Aug. 2010.
Li, Q., M. Rapp, J. Röttger, R. Latteck, M. Zecha, I.
Strelnikova, G. Baumgarten, M. Hervig, C. Hall, and
M. Tsutsumi, Microphysical parameters of mesospheric
ice clouds derived from calibrated observations of polar mesosphere summer echoes at Bragg wavelengthsof 2.8 m and 30 cm, J. Geophys. Res., 115, D00I13,
doi:10.1029/2009JD012271, 2010.
Lorentzen, D. A., J. Moen, K. Oksavik, F. Sigernes, Y.
Saito, and M. G. Johnsen (2010), In situ measurement of
a newly created polar cap patch, J. Geophys. Res., 115,
A12323, doi:10.1029/2010JA015710, 2010.
Milikh, G. M., A. G. Demekhov, K. Papadopoulos, A.
Vartanyan, J. D. Huba, and G. Joyce , Model for artificial ionospheric duct formation due to HF heating, Geophys. Res. Lett., 37, L07803, doi:10.1029/2010GL0426,
2010.
Nordblad, E. and T.B. Leyser, Ray tracing analysis of
L mode pumping of the ionosphere, with implications
for the magnetic zenith effect, Ann. Geophys., 28, 17491759, 2010.
Nozawa, S., Y. Ogawa, S. Oyama, H. Fujiwara, T. Tsuda,
A. Brekke, C. M. Hall, Y. Murayama, S. Kawamura, H.
Miyaoka, and R. Fujii, Tidal waves in the polar lower
thermosphere observed using the EISCAT long run data
set obtained in September 2005, J. Geophys. Res., 115,
A08312, doi:10.1029/2009JA015237, 2010.
Nygren, T. and Th. Ulich, Calculation of signal spectrum by means of stochastic inversion, Ann. Geophys.,
28,1409-1418, 2010.

38

Ogawa, Y., S.C. Buchert, A. Sakurai, S. Nozawa, R.
Fujii, Solar activity dependence of ion upflow in thepolar ionosphere observed with the European Incoherent Scatter (EISCAT) Tromsø UHF radar, J. Geophys.
Res.,115, A07310, doi:10.1029/2009JA014766, 2010.
Oksavik, K., V. L. Barth, J. Moen, and M. Lester(2010), On the entry and transit of high-density plasma
across the polar cap, J. Geophys. Res., 115, A12308,
doi:10.1029/2010JA015817, 2010.
Oyama, S., K. Shiokawa, J. Kurihara, T.T. Tsuda, S. Nozawa, Y. Ogawa, Y. Otsuka, and B. J. Watkins, Lowerthermospheric wind fluctuations measured with an FPI
during pulsating aurora at Tromsø Norway, Ann. Geophys., 28, 1847-1857, 2010.
Rinne, Yvonne, EISCAT Svalbard Radar Studies of
Meso-Scale Plasma Flow Channels in the polar cusp
ionosphere, PhD thesis, University of Oslo, 2010.
Rother, M., K. Schlegel, H. Lühr, and D. Cooke, Validation of CHAMP electron temperature measurements
by incoherent scatter radar data, Radio Sci., 45, RS6020,
doi:10.1029/2010RS004445, 2010.
Senior, A., M.T. Rietveld, M.J. Kosch and W. Singer,
Diagnosing Radio Plasma Heating in the Polar Summer Mesosphere using Cross-Modulation: Theory
and Observations, J. Geophys. Res., 115, A09318,
doi:10.1029/2010JA015379, 2010.
Shergill, H., T.R. Robinson, R.S. Dhillon, M. Lester, S.E.
Milan, and T.K. Yeoman, A statistical study of the spatial distribution of Cooperative UK Twin Located Auroral Sounding System (CUTLASS) backscatter power
during EISCAT heater beamsweeping experiments, J.
Geophys., Res., 115, A05307, doi:10.1029/2009JA014659,
2010.
Strelnikova, I., and M. Rapp, Studies of polarmesosphere summer echoes with the EISCAT VHF
and UHF radars: Information contained in the
spectral shape, Adv. Space Res., 45, 2, 247-259,
doi:10.1016/j.asr.2009.09.007, 2010.
Vickers, H., T. Robinson, and I. W. McCrea, A
method for improving plasma temperature estimatesfrom incoherent scatter analysis during artificial ionospheric modification experiments, J. Geophys. Res., 115,
A11316, doi:10.1029/2010JA015606, 2010.
Voiculescu, M., T. Nygren, A. Aikio, and R. Kuula,
An olden but golden EISCAT observation of a quiettime ionospheric trough, J. Geophys. Res., 115, A10315,
doi:10.1029/2010JA015557, 2010.

Wannberg U.G., Andersson H., Behlke R., Belyey V., Bergqvist P., Borg J., Brekke A., Delsing J., Eliasson L., Finch
I., Grydeland T., Gustavsson B., Haggstrom I., Harrison
R.A., Iinatti T., Johansson G., Johansson J., Johansson
J., La Hoz C., Laakso T., Larsen R., Larsmark M., Lindgren T., Lundberg M., Markkanen J., Marttala I., McCrea
I., McKay D., Postila M., Puccio W., Renkwitz T., Turunen E., van Eyken A., Vanhainen L.-G., Westman A.
and Wolf I., EISCAT_3D - A next-generation European
radar system for upper atmosphere and geospace research, Radio Science Bulletin, No 332, 75-88, 2010
Wild, P., F. Honary, A. J. Kavanagh, and A. Senior,
Triangulating the height of cosmic noise absorption:
A method for estimating the characteristic energy of
precipitating electrons, J. Geophys. Res., 115, A12326,
doi:10.1029/2010JA015766., 2010.
Wood, A. G. and Pryse, S. E., Seasonal influence on polar
cap patches in the high-latitude nightside ionosphere, J.
Geophys. Res., 115, A07311, doi:10.1029/2009JA014985,
2010.
Woodfield, E. E., J. A. Wild, A. J. Kavanagh, A. Senior,and S. E. Milan, Combining incoherent scatter radar
data and IRI-2007 to monitor the open-closed field
line boundary during substorms, J. Geophys. Res., 115,
A00I15, doi:10.1029/2010JA015751, 2010.

Xue Kun, Wu Jian, Xu Bin, Guo Lixin, Interpretationon the origin of enhanced ion acoustic line spectra in
the high ionosphere, Chin. J. Space Sci., 30(1), 29-34 (inChinese), 2010.
Xu Bin, Wang Zhange, Xu Zhengwen,Wu Zhensen, Wu
Jian, Wu Jun,Xue Kun, Che Haiqing, Yan Yubo, Observations of the heating experiments in the polar winterionosphere - Analysis in low region. Chinese Journal
Geophysics, 53(6), 1263-1268 (in Chinese), 2010.
Xu Bin, Wu Zhensen, Wu Jian, Che Haiqin,Wu Jun,
Xue Kun, 2D numerical simulation of the artificial ionospheric modification in polar region, Chinese Journal ofRadio Science, 25(1), 14-19, (in Chinese), 2010.
Xu Bin, Wang Zhange, Wu jun, Xu Zhengwen, Xue
Kun, Wu Jian, Observation of The Heating Experiments in the Polar Ionosphere in August, 2009,
Chinese Journal of Polar Research, 22, 4, 334-347, DOI:
10.3724/SP.J.1084.2010.00334, (in Chinese), 2010.
Zhang, S.-R., J.M. Holt, A.P. van Eyken, C. Heinselman, and M. McCready, IPY observations of ionospheric
yearly variations from high- to middle-latitude incoherent scatter radars, J. Geophys. Res., 115, A03303,
doi:10.1029/2009JA014327, 2010.

39

EISCAT Operations 2010
The EISCAT radars operate in two basic modes,
using approximately half the available observing
time for each. In the Special Programme mode,
users conduct individual experiments dedicatedto specific experiments and objectives. The resulting data are reserved for the exclusive use of theexperimenters for one year from the date of collection. Special programmes often make use of
the well developed pulse schemes and observing
modes of the Common Programme. EISCAT Common Programmes are conducted for the benefit of
the entire user community and the resulting data
are immediately available to all. The Common
Programme modes are developed and maintainedby EISCAT staff, and the overall programme ismonitored by the Scientific Oversight Committee(SOC). Common Programme operations are often conducted as part of the coordinated WorldDay programme organised by the International
Union of Radio Scientists (URSI) Incoherent Scatter Working Group (ISWG).
Common Programme One, CP-1, uses a fixedtransmitting antenna, pointing along the geomagnetic field direction. The three-dimensional velocity and anisotropy in other parameters are measured by means of the receiving stations at Kiruna
and Sodankylä (see map, inside front cover). CP-1
is capable of providing results with very good time
resolution and is suitable for the study of substorm
phenomena, particularly auroral processes whereconditions might change rapidly. The basic time
resolution is 5 s. Continuous electric field measurements are derived from the tri-static F-region
data. On longer time scales, CP-1 measurements
support studies of diurnal changes, such as atmospheric tides, as well as seasonal and solar-cycle
variations. The observation scheme uses alternating codes for spectral measurements.
Common Programme Two, CP-2, is designed tomake measurements from a small, rapid transmitter antenna scan. One aim is to identify wave-likephenomena with length and time scales comparable with, or larger than, the scan (a few tens ofkilometers and about ten minutes). The present
version consists of a four-position scan which is
40

EISCAT Svalbard radar antennas.

completed in six minutes. The first three positions
form a triangle with vertical, south, and south-east
positions, while the fourth is aligned with the geomagnetic field. The remote site antennas provide
three-dimensional velocity measurements in the Fregion. The pulse scheme is identical with that of
CP-1.
Common Programme Three, CP-3, covers a 10◦
latitudinal range in the F-region with a 17-position
scan up to 74◦ N in a 30 minute cycle. The observations are made in a plane defined by the magnetic meridian through Tromsø, with the remotesite antennas making continuous measurements at
275 km altitude. The coding scheme uses alternating codes. The principle aim of CP-3 is the mapping of ionospheric and electrodynamic parameters over a broad latitude range.
Common Programmes One, Two, and Three are
run on the UHF radar. Three further programmes
are designed for use with the VHF system. The
UHF and VHF radars are often operated simultaneously during the CP experiments. Such observations offer comprehensive data sets for atmospheric, ionospheric, and magnetospheric studies.
Common Programme Four, CP-4, covers geographic latitudes up to almost 80◦ N (77◦ N invariant latitude) using a low elevation, split-beam configuration. CP-4 is particularly suitable for studies
of high latitude plasma convection and polar cap
phenomena. However, with the present one-beamEISCAT VHF and UHF transmitter antennas, Tromsø.

configuration of the VHF radar, CP-4 is run witheither both UHF and VHF radars or with UHF
only in a two position scan.
Common Programme Six, CP-6, is designed for
low altitude studies, providing spectral measurements at mesospheric heights. Velocity and electron density are derived from the measurements
and the spectra contain information on the aeronomy of the mesosphere. Vertical antenna pointing is used.
Common Programme Seven, CP-7, probes highaltitudes and is particularly aimed at polar windstudies. The present version, with only one of the
VHF klystrons running, is designed to cover altitudes up to 1500 km vertically above Ramfjordmoen.
Equivalent Common Programme modes areavailable for the EISCAT Svalbard Radar. CP-1

is directed along the geomagnetic field (81.6◦ inclination). CP-2 uses a four position scan. CP-3
is a 15 position elevation scan with southerly
beam swinging positions. CP-4 combines observations in the F-region viewing area with fieldaligned and vertical measurements. Alternatingcode pulse schemes have been used extensively
for each mode to cover ranges of approximately
80 to 1200 km with integral clutter removal below 150 km. CP-6 is similar to the mainland radar
CP-6.
The tables on the next pages summarise the accounted hours on the various facilities for eachmonth and for each Common Programme mode
(CP) or Associate (SP).
Dr. Ingemar Häggström
Senior Scientist, EISCAT Scientific Association

41

2010

KST COMMON PROGRAMMES
2010
CP1
CP2
CP3
CP4
CP6
CP7
UP1
UP2
UP3
Total
%

Jan

Feb
Mar
5.5
94.5

Apr
May
39.5
39

Jun

Jul

Aug

Sept
12

Oct
60.5

Nov
59.5

60.5
6

59.5
6

413.5

36.5

5.5

36

37.5

1
63

36
4

37.5
4

76
7

63

450
44

5.5
1

94.5
9

45
4

39
4

63
6

Dec

%

Dec

Total Incl AA Target
93
94
84
197
199
143
107.5
109
82
157
160
168
117.5
123
325
108.5
112
234
253.5
257
219
20.5
1054.5
1055
1256
100

Total
310.5
413.5
0
0
116.5
62
188
0
0
0
62 1028.5
6100

Target%
30
16
40
16
0
12
0
10
11
20
18
18
0
0
0
100

KST SPECIAL PROGRAMMES
2010
CN
FI
GE
NI
NO
SW
UK
AA
Total
%

Jan

Feb

Mar
43

Apr

May

Jun

Jul
Aug
19.5

Sept
30.5

Oct

Nov

32.5
22.5
31.5

18.5
53.5

54
5

72
7
EI

26
16.5
6

91.5
9

0
0
FI
11.4

0
0
GE
6.56

12

96.5

12

40.5
24

39

161
15

311
29

3.5
24

CN
6.7

Target

97.5

164.5
107.5

130
12

47
4

NI
13.41

NO
25.91

3
11.5
14.5
1
SW
18.6

110
9
149.5
14

24
2

UK
17.43 %KST OTHER PROGRAMMES
2010
3P
EI
RU
TB
Total

Jan

Feb

Mar

5.5
1.5
0

7

Apr

May

Jun

Jul

Aug

Sept

Oct

Nov

Dec
3.5

60
13.5
73.5

0

0

0

Total
0
9
122
41
172

Target
35
25
139
41
240

0

0

60.5
3.5
64

Aug
Sept
37.5
76
14.5 149.5
0052 225.5

Oct
60.5
24
0
84.5

Nov
59.5
161
64
284.5

Dec
Total Target
62 1028.5
840
311 1054.5
1256
27.5
172
240
400.5
2255
2335

Oct
41
24

Nov
157.5
46
43.5
149.5
178

Dec
Total Target
119.5 965.5
984
229 712.6
747
29
219
254
94.5 1370.5
1400
166.5 1223.5
1406
70

0

0

24
27.5

KST CUMULATIVE TOTALS
2010
CP
SP
OP
Total

Jan
450
54
0
504

Feb
Mar
5.5
94.5
72
91.5
7
73.5
84.5 259.5

Apr
May
45
39
0
0
0
0
45
39

Jun
63
130
0
193

Jul
36
47
0
83

USAGE BREAKDOWN
2010
UHF
VHF
Heating
Passive UHF
ESR
Passive ESR

Jan
309.5
41
618
253.5

Feb
Mar
42.5 158.5
10.6
13
43.5
51
228
50.5
82

Apr
May
0.5
44.5
39

91

67

Jun
57
92
37
26
64

Jul
19.5
53

Aug
49.5
11.5
53
6

41.5

42

Sept
60
84
53
114.5
74
64

77.5
102.5

2010

ESR COMMON PROGRAMMES
2010
CP1
CP2
CP3
CP4
CP6
CP7
UP1
UP2
UP3
Total
%

Jan
1.5
185

Feb
2

Mar
62.5

Apr
May
39
39

Jun

Jul
24.5

Aug
Sept
30.5
3

62

186.5
29

2
0

62.5
10

39
6

39
6

62
9

Oct
39

Nov
39

39
6

39
6

63

24.5
4

30.5
5

66
10

Dec

Total
280
185
0
0
0
64
189
0
0
0
64
654
10
100

%

Target%
43
54
28
16
0
12
0
10
0
29
0
0
0
100

Dec

ESR SPECIAL PROGRAMMES
2010
CN
FI
GE
NI
NO
SW
UK
AA
Total
%

Jan

Feb

Mar

13.5
5
17
31.5

23.5

67
14

39.5
8

Apr

May

Jun

Jul

Aug

Sept

Oct

Nov

10
16

19.5

52

2

17

24

24.5

19.5
4

52
11

24.5
5

2
0

1.5
12.5
24
5

17
4

16
8
24
5

24
5

41

22.5

22
2.5
3.5
3

10.5
16
9
44.5

72
15

102.5
22

Total Incl AA Target
0
1
37
63.5
66
63
0
1
36
56
59
74
154
159
144
54
58
103
120
124
97
20.5
468
468
554
100

Nov

Dec

ESR OTHER PROGRAMMES
2010
3P
EI
RU
TB
Total

Jan

Feb

Mar

Apr

May

Jun

Jul

Aug

Sept

Oct
27.5

0

12
39.5

67
67

Total Target
27.5
35
0
25
9
9
82.5
83
0
119
152

Aug
Sept
30.5
66
24
24
0
0
54.5
90

Oct
39
24
39.5
102.5

Nov
39
72
67
178

Dec
Total Target
64
654
700
102.5
468
554
0
119
152
166.5
1241
1406

9
0

9

0

0

3.5
3.5

0

0

0

ESR CUMULATIVE TOTALS
2010
CP
SP
OP
Total

Jan
186.5
67
0
253.5

Feb
2
39.5
9
50.5

Mar
62.5
19.5
0
82

Apr
May
39
39
52
24.5
0
3.5
91
67

Jun
62
2
0
64

Jul
24.5
17
0
41.5

43

List of meetings 2010
EISCAT Annual Review Meeting EISCAT_3D_2 Preparatory Phase
ARM 2010 15–17 March, 2010, Björkliden, Project Meetings
SwedenGA1 6 October 2010, 1st General Assembly meeting of the EISCAT_3D_2 Preparatory Phase
project, Radisson Blu Hotel Arlandia, Arlanda, Sweden

EISCAT Council
Council 74th 3–4 June 2010, National Institute ofPolar Research, Tokyo, JapanEB1 21 October 2010, 1st Executive Board meeting, Clarion Hotel, Stockholm, Sweden

Council 75th 1–2 November 2010, British Antarctic Survey, Cambridge, UK

Kick-off 21–22 October 2010, Kick-off meeting for
the Preparatory Phase project, Clarion Hotel,
Stockholm, Sweden

EISCAT Council Advisory Group

Weekly Starting from 29 October 2010, weekly
Executive Board teleconferences

CAG 6th 26 April 2010, Vetenskapsrådet, Stockholm, Sweden
CAG 7th 2–5 October 2010, Finnish Meteorological Institute, Helsinki, Finland

EISCAT ScientificCommittee

Oversight

SOC 6th 25–26 March 2010, Solar-Terrestrial Environment Laboratory, Nagoya University,
Nagoya, Japan
SOC 7th 9–10 September 2010, Arctic and Antarctic Research Institute, St. Petersburg, Russia

44Staff celebrations 2010
ARM 2010
2 years (Silver pin) Elisabet Goth, Headquarters
5 years (Gold pin) Martin Langteigen, EISCAT
Svalbard Radar
20 years (Wrist watch) Inge Marttala, Kiruna site
25 years (Glass sculpture) Toivo Iinatti, Sodankylä site

Other
Retiring Inge Marttala, Kiruna site
Tarmo Laakso, Sodankylä site

45

Beynon medals
outstanding contributions to the scientific exploitation of incoherent scatter in Europe including the UK PUSCAT and MISCAT radars
and the radars of the EISCAT Scientific Association
5th Prof. Nobuo Matuura 2007 Awarded by theCouncil of the EISCAT Scientific Association
to Professor Nobuo Matuura. In recognitionof his contributions to the successful establishment of the EISCAT Svalbard Radar at
Longyearbyen and to the expansion of the
EISCAT Scientific Association to include nonEuropean members
The EISCAT Council awards distinguished persons the Sir Granville Beynon medal.

Recipients
1st Prof. Tor Hagfors 2002 Awarded to Professor
Tor Hagfors on 4th February 2002 for his outstanding services to the EISCAT Scientific Association and to Ionospheric Physics
2nd Prof. Tauno Turunen 2003 In recognition ofimportant contributions to the techniques of
Incoherent Scatter Radar and outstanding services to the EISCAT Scientific Association

6th Prof. Markku Lehtinen 2008 Awarded by theCouncil of the EISCAT Scientific Association
to Professor Markku Lehtinen. In recognitionof his seminal contributions to the development of advanced modulation techniques forincoherent scatter radars and to the mathematical foundations and implementation of effective incoherent scatter radar data analysis
systems
7th Dr. Gudmund Wannberg 2009 Awarded by
the Council of the EISCAT Scientific Association to Doctor Gudmund Wannberg. In
recognition of his persistent work for thetechnical development of EISCAT radars andhis invaluable contribution to the EU Design
Study project for the EISCAT_3D radars.
8th Prof. Asgeir Brekke 2010 Awarded by theCouncil of the EISCAT Scientific Association
to Professor Asgeir Brekke in recognitionof his pioneering work in polar ionosphereinvestigations with Incoherent Scatter Radarmeasurements and of his long-term efforts inadvocating EISCAT research worldwide.

3rd Prof. Jürgen Röttger 2004 In recognition ofoutstanding services to the EISCAT Scientific
Association including the establishment of
the EISCAT Svalbard Radar at Longyearbyen
4th Prof. Henry Rishbeth 2006 Awarded by theCouncil of the EISCAT Scientific Association
to Professor Henry Risbeth. In recognition of46

EISCAT organisational diagram, December 2010.

47

Hosts

Instruments

Sites

Headquarters

Council andCommittees

University of Oulu/SGO

Sodankylä

DFG
Germany

DeutscheForschungsgemeinschaft

STEL
Japan

Heating

UHF

Headquarters

Tromsø

IRF Kiruna

NIPR
National Institute ofPolar Research

NFR

VHF

NorwayNorgesforskningsråd

VR
SwedenVetenskapsrådet

United Kingdom

National
Environment
Research Council

NERC

NTIFIC AS
IE

ESR

Longyearbyen

CAG
Council Advisory
Group

University of Tromsø

EISCAT Council

Japan

Solar Terrestrial
Environment
Laboratory, Nagoya

KirunaSOC
Science OversightCommittee

Finland

China

SA
Suomen Akatemia

China
Research Institute ofRadiowave Propagation

CRIRP

CAT S
C
EIS

Funding
Agencies

CIATIONSO

EISCAT Scientific Association
December 2010
Council

Director

The Council consists of a Delegation with a maximumof three persons from each Associate.

Dr. E. Turunen

Council Advisory GroupP. R. of China
Prof. Q. Dong
Prof. J. Wu
Finland
Dr. A. Aikio
Dr. K. Kauristie
Dr. K. Sulonen
Germany
Prof. J. Röttger
Dr. K. ZachJapan
Dr. H. Miyaoka
Dr. S. Nozawa
NorwayProf. A. Brekke
Dr. B. Jacobsen
Dr. L. Lønnum
SwedenDr. T. Andersson
Prof. D. Murtagh
United Kingdom
Dr. I. McCrea
Dr. M. Schultz

The Council Advisory Group (CAG) prepares matters to
be brought to the Council.

Delegate

Mr. H. Andersson
Dr. T. Andersson
Prof. A. Brekke
Dr. K. Kauristie
Dr. I. McCrea
Dr. E. Turunen

Chairperson
Delegate
Delegate
Delegate

Head of Administration
Council Vice-Chairperson
Council Member
Council Chairperson
Council Member
Director

Executives
Senior Management

Delegate

Mr. H. Andersson
Dr. E. Turunen

Vice-Chairperson, Delegate

Site Leaders
Station Managers

Delegate

Scientific Oversight Committee
The EISCAT scientific community organises the Scientific Oversight Committee (SOC), under the guidanceof the Council.
Dr. N. BlagoveshchenskayaDr. S. Buchert
Dr. J. Chau
Dr. M. Kosch
Prof. C. La Hoz
Prof. R. Liu
Dr. Y. Ogawa
Prof. M. Rapp
Dr. T. Ulich

Head of Adm., Deputy Dir.
Director

External member
SwedenExternal member
United Kingdom
NorwayChairperson, P. R. of China
Japan
Germany
Finland48

Mr. H. Boholm
Mr. R. Jacobsen
Mr. J. Markkanen
Dr. M. Rietveld
Mr. L.-G. Vanhainen

EISCAT Svalbard Radar
Tromsø Radar
Sodankylä Site
Tromsø Heating
Kiruna Site

EISCAT staff at the Annual Review Meeting, 15–17 March 2010, at Björkliden, Sweden.

50

Appendix:
EISCAT Scientific Association
Annual Report, 2010

51

EISCAT Scientific Association Annual Report 2010

EISCAT Scientific Association
Registered as a Swedish non-profit organisation
Organisation number: 897300-2549
Annual report for the financial year 2010-01-01 – 2010-12-31
The EISCAT Council and the Director for the Association submits herewith the annual reportfor 2010.
Content
Administration report
Profit and loss accounts
Balance sheet
Statement of cash flows
Notes

Page
1
5
6
7
8

52

EISCAT Scientific Association Annual Report 2010

ADMINISTRATION REPORT
Ownership, organisation and objective
The EISCAT Scientific Association was established in 1975 through an agreement between six
European organisations. Japan joined in 1996 and the Peoples Republic of China in 2007.
The EISCAT Associates at 2010-12-31 are: China Research Institute of Radiowave Propagation(Peoples Republic of China), Deutsche Forschungsgemeinschaft (Germany), National
Institute of Polar Research (Japan), Natural Environment Research Council (United Kingdomof Great Britain and Northern Ireland), Norges forskningsråd (Norway), Solar-Terrestrial
Environment Laboratory, Nagoya University (Japan), Suomen Akatemia (Finland), andVetenskapsrådet (Sweden).
A new EISCAT Agreement came into force 2007-01-01, with all Associates making long term
funding commitments to the Association. The Association has its formal seat in Kiruna,
Sweden, and is registered as a non-profit organisation.
The aim of the Association is to make significant progress in the understanding of physicalprocesses in the high latitude atmosphere by means of experimental programmes generally
conducted using the incoherent scatter radar technique, which may be carried out as part ofwider international projects. For this purpose, the Association has developed, constructed,
and now operates, a number of radar facilities at high latitudes. At present, these comprise asystem of stations at Tromsö (Norway), Kiruna (Sweden), Sodankylä (Finland), andLongyearbyen (Svalbard).
The Association is fully funded by the Associates but additional operations may also be
funded by short term additional contributions from both Associate and non-Associatebodies. Depending on the available funding, scientific priorities and operational targets areadjusted on an annual basis.
The EISCAT Council is charged with the overall administration and supervision of the
Association's activities. The Council appoints a Director, who is responsible for the daily
management and operation of the facilities of the Association.
Operation and scientific development
The EISCAT Radars delivered a full programme of operations for the user community andoperated reliably throughout the year with only minor interruptions due to equipment oroperational problems.
The various EISCAT radars operated for a total of 3 496 accounted hours (3 688 hours in2009).
The UHF tristatic runs, first envisaged to not be possible after July 2010, could continue also
after that date since the mobile operators that bought that frequency allocation did not start
using it during the year. Consequently, some Common Programmes as well as Special

-2-

53

EISCAT Scientific Association Annual Report 2010

Programme could be run in the tristatic mode (transmit/receive in Tromsö and receive onlyin Kiruna and Sodankylä).
Common Programmes amounted to 42% (43%) of the operations. Special Programmes
amounted to 37% (40%) and other operations amounted to 21% (17%) of the total hours.
Scientists from France, Ukraine and Russia paid for the use of the facilities. Totally
254.5 hours (298.5 hours) were run on behalf of these countries. Both Ukraine and Russia
have Affiliate agreements. Additionally, the European Space Agency (ESA) used theinfrastructure for a coordinated tracking campaign of objects PROBA-1, METOP-A, JASON_2,
GRACE-1, ENVISAT and CRYOSAT_2 in November and December. Totally 28.27 hours wererun on behalf of, and paid by, ESA.
The EISCAT_3D planning continued during the year and the EU Framework Programme 7 bid
for a preparatory phase, submitted in December 2009, was successful such that a new EU
supported project, the FP7 EISCAT_3D_2 preparatory phase could start 2010-10-01. It is afour year project with a total budget volume of 6 MEUR and eight partners. EISCAT is both apartner and coordinator for the project. The budgeted expected support from EU for the
EISCAT involvement amounts to 1.25 MEUR spread over the four years. The EU grant for thewhole project is 4.5 MEUR, which is channelled through the coordinator.
The goal of the preparatory phase project is to resolve the remaining legal, financial andtechnical questions which must be addressed before the construction of the EISCAT_3D
system.
A new development undertaken in the year was the project proposed by the Chinese
Associate, China Research Institute of Radiowave Propagation (CRIRP), to build a third
antenna system on Svalbard with dual mode capabilities. The antenna would be used for
EISCAT regular radar use and for Chinese operations such as coordinated VLBI
measurements together with mainland China antennas. The EISCAT involvement is to do theinitial feasibility studies for a possible build on Svalbard. The work is contracted out toconsultants and the cost is reimbursed from CRIRP.
Future operation and scientific development
During 2011, EISCAT will continue to support the wide range of existing and new
programmes proposed by the various Associates’ scientific communities, including thehosting of user-supplied equipment.
Tristatic runs will likely be possible to be done some more months and will be encouraged.
The small Demonstrator receive-only array built in connection with the previous EISCAT_3D
project, the design study, will be tilted downwards such that the array points at the E region
and meteor heights 80-120 km instead of its present direction to F-region around 300 km
above the VHF transmitter in Tromsö. If the sensitivity is adequate, it could be a valuable
option for many users with interest in the lower regions. The modification will be readysummer 2011.

-3-

54

EISCAT Scientific Association Annual Report 2010

The three other radar systems, UHF in monostatic mode, VHF and the Svalbard Radarcontinues undisturbed. The Heating facility has been modernised and can also now be used
as a magnetospheric radar.
The work of the Council and its committees
The Council had two ordinary meetings under the leadership of the Chairperson, Dr. Kirsti
Kauristie: in June, Tokyo, Japan and in November, Cambridge, United Kingdom. At the end ofyear, the Council Chairpersonship was taken over by Dr. Tomas Andersson, Vetenskapsrådet,Sweden. He will serve for two years. The Council Advisory Group had two meetings under
the leadership of the Chairperson, Dr. Kirsti Kauristie: in April, Stockholm, Sweden and in
October, Helsinki, Finland. The Scientific Oversight Committee had two meetings under theleadership of the Chairperson, Prof. Ruiyuan Liu: in March, Nagoya, Japan and in September,
St. Petersburg, Russia,
Council considered regular business matters, including the continued EISCAT_3D work andthe third antenna proposal. Council decided also to assign 200 hours peer-reviewed pool oftime (PP programme) opened for users around the world and to allocate 100 kSEK annuallyfor a regularly occurring radar school. Both actions were implemented in the 2011 budget.
The financial implications from potential departure of Associates in 2012 resulted inproactive measures both involving work in improving the income side as well as reducing
operating costs to be included in the 2012 budget onwards.
The transfer of the UK Associateship from the Science and Technology Facilities Council(STFC) to the Natural Environment Research Council (NERC) was finalised during the firstmonths of the year meaning that NERC is from 2010-01-01 the UK Associate.
Budget development during the year
The 2010 operations ended just below the operating target set for the year and theoperations went without any major technical issues. The application for the EISCAT_3D
preparatory phase was done partially by external writers, paid as consultancy. The
management travel continued at a very high rate. Income from bank interest continued on alow level. Active placements generated reasonable return that compensated from themarginal bank interest income. The income side continued to benefit from the relatively
weak SEK-currency and generated, due to the Associate commitments in local currencies
and annual payments in the first half of the year, additional income. The strengthening of
SEK during the latter part of the year created though some exchange rate losses.
The long-term budget plan
The long-term budget plan is difficult due to the current known funding shortage from 2012
onwards. For 2011, we plan for a normal year and the overall operating target can likely bemaintained. The 2012 budget will include substantial cost reductions, including a reduced
staff complement, and the operations from then on will be more directly tied to received
contributions.
The result for 2010 and the deficit handling
The year was balanced by covering the deficit, -83 kSEK, from the Restructuring reserve.

-4-

55

EISCAT Scientific Association Annual Report

PROFIT AND LOSS ACCOUNTS
in thousands of Swedish Crowns
Note 1

Associate contributions
Other operating income

Note 2

Operation costs
Administration costs
Personnel costs
Depreciation of fixed assets

Note 3Operating profit/loss
Interest income
Other financial income and cost
Own reserves and funds

Note 4

Profit/loss after financial items
Appropriations
Transfer from funds invested

Note 5Note 6

Net profit/loss for the year

‐ ‐

56

2010
24 2483 219
27 4672009
26 5866 180
32 766‐6 243‐4 413‐17 854‐1 214‐29 724‐5 257‐4 517‐17 706‐2 198‐29 677‐2 257

3 089

52
‐41
949
960

85
‐622
‐1 335‐1 871‐1 297

1 217

83
1 214
1 297

‐3 415
2 198‐1 21700

EISCAT Scientific Association Annual Report

BALANCE SHEETin thousands of Swedish Crowns
2010

2009

3 557
748
1 664
5 968

3 843
821
2 099
6 764

3 050
1 129
24 71128 8893 871
640
19 22223 73334 85830 496ASSETS
Fixed assets
Tangible fixed assets
Buildings
Radar systems
Equipment and tools

Note 7

Current assets
Receivables
Prepayments and accrued income
Cash at bank and in hand

Note 8Note 9Total assets
CAPITAL AND LIABILITIESCapitalFunds invested
Funds held on reserve

Note 115 968
17 31223 2806 764
18 76325 526Long term liabilities
Long term liabilities

Note 1200Note 13

11 4250152
11 578

4 469
155
345
4 970

34 85830 496

0

0

none

none

Note 10

Current liabilities
Liabilities, trade
Provisions
Other liabilities

Note 14

Total capital and liabilities
Pledged assets
Contingent liabilities

‐ ‐

57

EISCAT Scientific Association Annual Report

STATEMENT OF CASH FLOWS
in thousands of Swedish Crowns
2010

2009

‐2 257
1 214

3 089
2 198

52
‐57
15

85
‐658
36

Increase/decrease of receivables
Increase/decrease of prepayments and accrued income
Increase/decrease of creditors and liabilities

821
‐489
6 608

‐2 148‐30‐2 252

Cash flow from operations

5 907

321

Investment activities
Investments in tangible assets‐419‐1 469Cash flow from investment activities‐419‐1 469Cash flow for the year

5 488

‐1 148Liquid assets at the beginning of the year

19 22220 370Liquid assets at the end of the year

24 71119 222

Operating activities
Operating result before financial items
Transfer from funds invested
Interest received
Currency exchange rate changes
Extra ordinary income and cost

‐ ‐

58

EISCAT Scientific Association Annual Report
2010

2009

Salaries and emoluments paid to the Director

1 286

1 240

Other personnel, employed and provided
via site contracts

10 971

11 031Social security contributions amounted toof which for pension costs

4 106
2 086

3 944
1 992

NOTES
Note 1 Accounting principles

Personnel costs in total

The accounting and valuation principles applied are consistent with theprovisions of the Swedish Annual Accounts Act and generally accepted
accounting principles (bokföringsnämnden allmänna råd ochvägledningar).
All amounts are in thousands of Swedish kronor (SEK) unless otherwise
stated.
Receivables
Receivables are stated at the amounts estimated to be received, basedon individual assessment.
Receivables and payables in foreign currencies
Receivables and payables in foreign currencies are valued at the closing
day rate. Where hedging measures have been used, such as forwarding
contracts, the agreed exchange rate is applied. Gains and losses relating
to operations are accounted for under other financial income and cost.
Bank accounts in foreign currencies
Bank balances in foreign currencies are valued at the closing day rate.
Fixed assets
Tangible fixed assets are stated at their original acquisition values after
deduction of depreciation according to plan. Assets are depreciatedsystematically over their estimated useful lives. The following periods ofdepreciation are applied: Buildings 5 ‐ 50 years, Radar systems 3 ‐ 20years and Equipment and tools 1 ‐ 5 years.

The Director, Dr. Esa Turunen, started his employment 2009‐01‐01. His
employment contract with Council is for three years.
Of the pension costs, 333 kSEK (320 kSEK) relates to the Director. He
and all other directly employed staff are included in ITP like
occupational pension plans. For the personnel provided via site
contracts, the pension plans are handled by their respective employer.
The members of the board (EISCAT Council) and members ofcommittees, who represents Associates, do not receive remunerations
from the Association. Travel expenses in connection with Council andcommittee meetings are normally covered by the Associates. For theCouncil Advisory Group, the Association cover meeting and travel costs.
Salaries and emoluments and average number of staff per country
Finland
Salaries and emoluments
Average number of staff ‐ men and women

1 029
2+0

1 528
3+0

Norway (including Svalbard)
Salaries and emoluments
Average number of staff ‐ men and women

5 818
10 + 05 370
9+0SwedenSalaries and emoluments
Average number of staff ‐ men and women

5 410
7+1

5 372
8+1

Note 2 Associate contributions
The Associates contributed to the operation during the year inaccordance with the agreement. The commitments are in local
currencies. The received contributions have been accounted in SEK.
2010
CRIRP (P. R. of China)
2 849
DFG (Germany)
1 732
NIPR (Japan)
1 768
RCN (Norway)
5 745
SA (Finland)
3 371
STFC (United Kingdom)
3 384
VR (Sweden)
5 400
24 248
Accumulated contributions status as of 2010‐12‐31
1976 ‐ 2010
Previous Associates
190 074
CRIRP (P. R. of China)
13 457
DFG (Germany)
190 480
NIPR (Japan)
68 671
RCN (Norway)
140 121
SA (Finland)
62 188
STFC (United Kingdom)
217 775
VR (Sweden)
113 429996 196Note 3 Personnel costs and average number of employees
The Association employs directly the Headquarters staff, currently about
six positions, including the Director. The Headquarters is located in
Kiruna, Sweden. The personnel working at the Kiruna (Sweden),
Sodankylä (Finland), Svalbard and Tromsö (Norway) sites are not
employed by the Association. Instead, the personnel are provided via
site contracts by the Swedish Institute of Space Physics (Kiruna site
staff), Oulu University (Sodankylä staff) and Tromsö University (Tromsö
and Svalbard staff). The Association refunds all expenses related to theprovided staff, as well as an additional overhead.

‐ ‐

59

Members of the board and Directors at year‐end ‐ men and women
The board consist of delegations from every Associate country eachhaving a Delegate (formal member) and up to two Representatives.
Board members (EISCAT Council)
Directors

12 + 4
1+0

12 + 4
1+0

Capital Operating reserve
Budgeted transfer to the reserve
Transfer from the reserve
Investments made

‐884
419
‐419

‐1 6141 469‐2 040External projects reserve
Project(s) complete, funds released

0

1 504

Restructuring reserve
Budgeted restructuring costs

0

1 500

‐28
109

‐28
9

Note 4 Own reserves and funds
Transactions involving own reserves and funds.

Spare parts reserve
Budgeted transfer to the reserve
Transfer from the reserve

EISCAT Scientific Association Annual Report

Investment fund
Budgeted transfer to the fund
Surplus fund
Budgeted transfer from the fund
Budgeted transfer to the fundSum own reserves and funds

2010

2009

0

‐2 0004 196‐2 4454 062‐4 196949‐1 33520102009

Note 8 Prepayments and accrued income
The main buildings and systems insurance for 2010 was paid in
December. Costs relating to the Antenna III feasibility work wereinvoiced in February 2011 and the EISCAT_3D_2 project costs spent in2010 will be claimed from EU in April 2012.
Prepaid rents
Prepaid insurances
Accrued income
Other items

Note 5 Appropriations
The outcome for this year became a deficit relative to the budget
amounting to ‐83 kSEK. The deficit was covered by own reserves fromthe surplus fund. The 2009 outcome resulted in a surplus (3 415 kSEK),
which was put in the investment fund.

92
139
462
437
1 129

91
460
0
89
640

24 7092
24 71119 2202
19 222

3 557
748
1 664
5 968

3 843
821
2 099
6 764

Note 9 Bank balances status
NordeaCash in hand

Note 6 Transfer from funds invested
The depreciation cost is covered by funds from Capital ‐ funds invested
Note 10 Funds invested status
Note 7 Tangible fixed assets

Buildings
Radar Systems
Equipment and Tools

Changes in tangible fixed assets during 2010.
Buildings
Opening acquisition value
Acquisitions during the year
Disposals during the year
Closing acquisition value

42 3748
042 38242 237137
042 374‐38 531‐295
0‐38 825‐38 242‐289
0‐38 531

3 557

3 843

244 48459
0
244 542244 381103
0
244 484‐243 662‐132
0‐243 795‐242 340‐1 3230‐243 662

748

821

33 057352‐398
33 01131 9251 229‐98
33 057‐30 958‐787
398‐31 347‐30 283‐586‐89‐30 958

Closing residual value

1 664

2 099

Sum tangible fixed assets

5 968

6 764

Opening accumulated depreciation
Depreciations during the year
Disposals during the year
Closing accumulated depreciation
Closing residual value
Radar systems
Opening acquisition value
Acquisitions during the year
Disposals during the year
Closing acquisition value

Note 11 Funds held on reserve
Investments were made a bit below the budgeted expectation. Morespare parts than budgeted were acquired. Both actions were budget
neutral since the differences were covered by reserve transfers. The
deficit for this year (‐83 kSEK) were taken from the surplus fund. The
other transfers were as budgeted.
Capital operating reserve
Equipment repair fund
External projects reserve
Investment fundRestructuring reserve
Spare parts reserve
Surplus fund

1 834
754
0
7 971
4 101
290
2 362
17 312

1 369
754
0
7 971
4 101
371
4 196
18 763Note 12 Long term liabilities
Opening accumulated depreciation
Depreciations during the year
Disposals during the year
Closing accumulated depreciation
Closing residual value
Equipment and tools
Opening acquisition value
Acquisitions during the year
Disposals during the year
Closing acquisition value
Opening accumulated depreciation
Depreciations during the year
Disposals during the year
Closing accumulated depreciation

No long term liabilities. The Association is fully funded by the Associates.

Note 13 Liabilities, trade
The EISCAT_3D_2 preparatory phase project started 2010‐10‐01. The
project is financed by EU's European Commission through the
Framework Programme 7 scheme. The contract stipulates that apercentage of the total financing is withheld as contingency and kept ina guarantee fund with the Commission. The first prefinancing, minus thecontingency, were received in October. The guarantee fund will be
released at the end of the project, 2014‐09‐30.
EISCAT_3D_2 guarantee fund, whole project
EISCAT_3D_2 prefinancing, EISCAT share
Liabilities, trade

2 023
5 120
4 282
11 425

0
0
4 469
4 469

Note 14 Provisions
None in 2010. In 2009 the provision referred to an errorounus costdebit.
Provisions

‐ ‐

60

0

155

ElSCAT Scientific Association Annual Report 2010

Helsinki 2011-05-31

Dr. Tomas Andersson

ｊｾｖ＠

Dr. Hiroshi Miyaoka

Dr. Michael Schultz

Dr. Kati Sulonen

Prof. Jian Wu

Dr. Karin Zach

ｾ｣

｟Ｍ

Ｍ

Dr. Esa Turunen
Director

Our audit report was issued on 2011-06)3

r1JL

Mrs. Annika Wedin

Authorised Public Accountant- 10 -

61

p-wc
Audit report
To the council of EISCAT Scientific Association
Corporate identity number 897300-2549

I have audited the annual accounts, the accounting records and the administration of the council andthe director of EISCA T Scientific Association for the year 20 I O. These accounts and theadministration of the association and the application of the Annual Accounts Act when preparing theannual accounts are the responsibility of the council and the director. My responsibility is to express
an opinion on the annual accounts and the administration based on my audit.
I conducted my audit in accordance with generally accepted auditing standards in Sweden. Thosestandards require that I plan and perform the audit to obtain reasonable assurance that the annual
accounts are free of material misstatement. An audit includes examining, on a test basis, evidence
supporting the amounts and disclosures in the accounts. An audit also includes assessing theaccounting principles used and their application by the council and the director and significant
estimates made by the council and the director when preparing the annual accounts as well as
evaluating the overall presentation of information in the annual accounts. As a basis for my opinion
concerning discharge from liability, I examined significant decisions, actions taken and circumstancesof the association in order to be able to determine the liability, if any, to the council or the director. I
also examined whether any council member or the director has, in any other way, acted incontravention of the Annual Accounts Act or the statutes. I believe that my audit provides a reasonablebasis for my opinion set out below.
The annual accounts have been prepared in accordance with the Annual Accounts Act and give a trueand fair view of the association's financial position and results of operations in accordance withgenerally accepted accounting principles in Sweden.
The statutory administration report is consistent with the other parts of the annual accounts.
The council and the director have not acted in contravention of the statutes.

ｇＧ ｾ Ｑ Ｚ ｾ＠
A(&.--w edin
Authorized Public Accountant

62

63

Report 2010 of the EISCAT Scientific Associationc EISCAT Scientific Association
EISCAT Headquarters
Box 812, SE-981 28 Kiruna, Sweden
Scientific contributions: EISCAT Associates and staff

64

CAT SCEISCIATIONSO

NTIFIC AS
IE

The EISCAT Associates
December 2010

CRIRP

China Research Institute of Radiowave Propagation
China
www.crirp.ac.cn

DFG

Deutsche Forschungsgemeinschaft
Germany
www.dfg.de

NERC

Natural Environment Research Council
United Kingdom
www.nerc.ac.uk

NFR

Norges forskningsråd
Norwaywww.forskningsradet.no

NIPR

National Institute of Polar ResearchJapanwww.nipr.ac.jp

SA

Suomen Akatemia
Finlandwww.aka.fi

STEL

Solar Terrestrial Environment Laboratory, NagoyaJapan
www.stelab.nagoya-u.ac.jp

VR

Vetenskapsrådet
Swedenwww.vr.seEISCAT Scientific Association
Headquarters
EISCAT Scientific Association
Box 812
SE-981 28 Kiruna, Sweden
Phone: +46 980 79150
Fax: +46 980 79159
www.eiscat.se

Sites
KirunaEISCAT Kiruna Site
Box 812
SE-981 28 Kiruna, Sweden
Phone: +46 980 79136
Fax: +46 980 29276

Longyearbyen
EISCAT Svalbard Radar
Postboks 432
N-9171 Longyearbyen, Svalbard
Phone: +47 790 21236
Fax: +47 790 21751

Sodankylä
EISCAT Sodankylä Site
Tähteläntie 54B
FIN-99600 Sodankylä, Finland
Phone: +358 16 619880
Fax: +358 16 610375

Tromsø
EISCAT Tromsø Site
Ramfjordmoen
N-9027 Ramfjordbotn, Norway
Phone: +47 776 20730
Fax: +47 776 20740